HARVARD UNIVERSITY. LIBRARY OF THE MUSEUM OF COMPARATIVE ZOOLOGY. PROCEEDINGS OF THE American Philosophical Society HELD AT PHILADELPHIA FOR PROMOTING USEFUL KNOWLEDGE VOLUME LI 1912 PHILADELPHIA THE AMERICAN PHILOSOPHICAL SOCIETY 1912 Press of The new Era printing companx lancaster pa CONTENTS. Determination of the Depth of the Alilky Way. By T. J. J. See i Contraband of War. By John Bassett Moore i8 The Legendary and Myth-making Process in Histories of the American Revolution. By Sydney G. Fisher 53 Phylogenetic Association in Relation to the Emotions. By George W. Crile, M.D 76 The Nature of the Japanese Verb, So-called. By Benjamin Smith Lyman 91 The Validity of the Law of Rational Indices, and the Analogy between the Fundamental Laws of Chemistry and Crystal- lography. By Austin F. Rogers 103 Dynamical Theory of the Globular Clusters and of the Cluster- ing Power Inferred by Herschel from the Observed Figures of Sidereal Systems of High Order. By T. J. J. See 118 The Classification of the Black Oaks. By William Trelease 167 Heredity of Feeble-mindedness. By Henry H. Goddard 173 The Heredity of Epilepsy Analyzed by the Mendelian Method. By David Fairchild Weeks 178 Is the Control of Embryonic Development a Practical Problem? By Charles R. Stockard 191 An Avian Tumor' in its Relation to the Tumor Problem. By Peyton Rous, M.D 201 The Protein Poison. By Victor C. Vaughan, M.D 2c6 Some Geochemical Statistics. By Frank Wigglesworth Clarke 214 Thermal Relations of Solutions. By William Francis Magie 235 New Magnetic Charts of the Indian Ocean. By L. A. Bauer. . 240 The Diary of a Voyage to the L'nited States, by Moreau de Saint-Mery. By Stewart L. Mims 242 The Classification of Carbon Compounds. By Marston Tay- lor BoGERT 252 iii IV CONTENTS. The Treaty-making Power of the United States and the Methods of its Enforcement as AfTecting the Pohce Powers of the States. By Charlf-S H. Burr 271 The Formation of Coal Beds. III. By John J. Stevexson. . 423 An AutocolHmating Mounting for a Concave Grating. By HoR.\CE Clark Richards 554 The Objective Prism. By Edward C. Pickerinc; 564 Notes on Plates of Nova Geminorum of 191 2 taken with the Bruce Spectrograph of the Yerkes Observatory. By Storrs B. Barrett , 568 Relations Between the Spectra and Other Characteristics of the Stars. By Henry Norris Russell 569 Some Former Members of the American Philosophical Society. By Thomas Willing Balch 580 Minutes iii-.vi.v Obituary Notices of Members Deceased Jules Henri Poincare iii For Corrigenda see page 603. PROCEEDINGS OF THE American Philosophical Society HELD AT PHILADELPHIA FOR PROMOTING USEFUL KNOWLEDGE Vol. LI. January-March, 191 2. No. 203. CONTENTS. Determination of the Depth of the Milky Way. By T. J. J. See I Contraband of War. By John Bassett Moore 18 Stated Meeting, January 5, igi2 Hi Stated Meeting, Febmary 2, igi2 iv Stated Meeting, March i, igi2 viii PHILADELPHIA THE AMERICAN PHILOSOPHICAL SOCIETY 104 South Fifth Street 1912 American Philosophical Society General Meeting — April 18-20, 1912 The General Meeting of /912 will be held on April iSth to 20th, beginning at 2 p. m. on Thursday, April i8th. Members desiring to present papers are requested to send to the Secretaries, at as early a date as practicable, and not later than April 10, 1912, the titles of these papers, so that they may be announced in the final programme which will be issued immediately thereafter, and which will give in detail the arrange- ments for the meeting. Papers in any department of science come within the scope of the Society, which, as its name indicates, embraces the whole field of useful knowledge. The Publication Committee, under the rules of the Society, will arrange for the immediate publication of the papers pre- sented. I. MINIS HAYS ARTHUR W. GOODSPEED AMOS P. BROWN HARRY F. KELLER Secretaries. Members who have not as yet sent their photographs to the Society will confer a favor by so doing; cabinet size preferred. It is requested that all correspondence be addressed To THE Secretaries of the AMERICAN PHILOSOPHICAL SOCIETY 104 South Fifth Street Philadelphia, U. S. A PROCEEDINGS OF THE AMERICAN PHILOSOPHICAL SOCIETY HELD AT PHILADELPHIA FOR PROMOTING USEFUL KNOWLEDGE Vol. LI January-March, 1912 No. 203 DETERMINATION OF THE DEPTH OF THE MILKY WAY. By T. J. J. SEE. {Read January 5, 1912.) Introductory Remarks. The problem of determining the depth of the Milky Way, as accurately as possible, is one which has now engaged my attention for over twenty years, and I will therefore take this occasion to bring together the results at which I have arrived, partly because they are of high general interest, and partly because the progress thus made will prove instructive as to the methods which must be adopted for the measurement of the distances of the most remote objects of the sidereal universe. Here we have to deal with dis- tances so immense that the method of annual parallaxes, commonly used for the stars comparatively near the sun, utterly fails; and recourse must be had to other methods which will serve for the greatest distances to which our modern giant telescopes can penetrate. Alpha Centauri, the nearest of the fixed stars, was also the first to be successfully measured for parallax, by Thomas Henderson, of the Cape of Good Hope, in 1831 ; but the work was not reduced till January, 1839, and meanwhile Bessel had measured the parallax of 61 Cygni in 1838 and promptly published the result of his triumph. PROC. AMER. PHIL. SOC. , LI. 203 A, PRINTED MARCH 16, I9I2. 2 SEE— DETERMINATION OF THE [Januarys. Of late years astronomers have given greatly increased attention to "the question of the distances of the stars, and systematic campaigns of the most laborious kind have been carried on by Gill ; Elkin and Chase, of Yale; Kapteyn, of Groningen ; and Schlesinger, at the Yerkes Observatory, Chicago. Some 350 stars have now been studied by the standard method of parallaxes, and for most of these objects, perhaps about 200 in number, fairly satisfactory data have been deduced ; but the method can be extended only to stars within less than 100 light-years of our sun, and is therefore very limited in its applicability, owing to the small diameter of the earth's orbit, and the insensible effects of the annual displacements resulting from the orbital motion of our planet. As nature herself has fixed the limits of this method, astronomers have naturally cast about for other methods of greater generality and have finally developed processes of surprising power, of which an account will be given in the present paper. § I. Outline of the Methods Adopted. Among previous investigators who have occupied themselves with the difficult problem of the profundity of the Milky Way the first place will be universally assigned to the incomparable Sir Wil- liam Herschel, who extended his researches over many years, and reached results which were for a time accepted, but have been rejected for three quarters of a century, and yet are now proved to be essentially correct. It is very remarkable and exceedingly unfor- tunate that Herschel's conclusions have been generally rejected by his son, Sir John Herschel, and other astronomers during the past seventy-five years. But before discussing the circumstances which led to this outcome I shall recall the modern attempts at the solution of the problem of determining distances in the Milky Way. After the spectroscope came into use and Huggins had applied Doeppler's principle to the motion in the line of sight (1868) it was pointed out by Fox Talbot in 1871 (Brit. Assoc. Report, 1871, p. 34, Pt. II.) that the possibility existed of determining the absolute dimensions of the orbit of a pair of binary stars which had a known 19I2-] DEPTH OF THE MILKY WAY. 3 angular dimension in the sky, and thus parallaxes might be found of systems very remote from the earth. In 1890, while a post- graduate student at the University of Berlin, I developed this method still further, and showed how it could be used also to test the accu- racy of the law of universal gravitation in the stellar systems. The spectroscopic method then outlined was brought to more general form in 1895, and it at once occurred to me to point out its use for measuring the distance of clusters in the Milky Way (A. N. 3,323), as more certain than Herschel's method of star gauges. Our age is one of rapid improvement in all scientific processes, and during the past sixteen years naturally much progress has been made in double-star astronomy, as well as in our knowledge of nebulae and clusters. On looking more closely into the spectroscopic method, which in 1895 had been shown to be applicable to objects 1,000 light-years from the sun, and might thus include all suitable double stars within this sphere, I became convinced that while it is a great theoretical advance over the old method of parallaxes, it still is quite inadecjuate for finding the distances of the most remote objects in the sidereal universe. Accordingly in 1909 I returned to the improvement of Herschel's method as the most promising, for the determination of the distances of the most remote objects. Here are the grounds for this decision : 1. It was noticed, as remarked by Burnham, that revolving double stars are rare, if not unknown, in clusters, and among the star-clouds of the Milky Way- — ^not because such systems are not present in these masses of stars, but because they cannot be separated, owing to the great distances at which these masses of stars are removed from us. 2. When double stars cannot be clearly separated in the tele- scope they cannot be used for parallax by the spectroscopic method ; and thus the spectroscopic method, while having a wider range of application than the method of parallaxes, in something like the ratio of the size of the double star orbit to that of the orbit of the earth, is yet applicable only to stars within about 1,000 light-years of our sun. 4 SEE— DETERMINATION OF THE [Januarys. 3. It will l)c shown below that the most remote stars are sepa- rated from us by a distance of at least 1,000,000 light-years, and as this space is a thousand times that to which the spectroscopic method may be applied, it follows that there is no way of fatliom- ing these immense distances except by the improvement of the method of Ilerschel. And just as in my " Researches on the Evolution of the Stellar Systems," \'ol. II., 1910, p. 638, I had been able to adduce sub- stantial grounds for returning to the vast distances calculated by Herschel. so also during the past year I have been able to add to the proof there brought forward, and will proceed, to develop it in the present paper, §2. Hersciiel's JNIetiiod Depending on the Space Penetrating Power of Telescopes. In his celebrated star gauges Herschel employed a twenty- foot reflector of 18 inches aperture, and calculated the space-penetrating power of such an instrument from the ratio of the aperture of the telescope to that of the pupil of the eye. The comparative distance to which a star would have to be removed in order that it may appear of the same brightness through the telescope as it did before to the naked eye may thus be calculated. Herschel found the pow-er of this 20-foot reflector to be 75 ; so that a star of 6th magnitude removed to 75 times its i)rcscnt distance would therefore still be visible, as a star, in the instrument. Admitting such a 6th magnitude star to give only a hundredth part of the light of the standard first magnitude star, it will follow that the standard star could be seen as a sixth magnitude star at ten times its present distance ; and if we then multiply by the sjiace penetrating power, we get 750 as the distance to which the standard star could be removed anrl still excite in the eye, when viewed through the telescope, the same impression as a star of 6th magni- tude does to the naked eye. Thus if Alpha Centauri be distant 4.5 light-years, it would be visible in Herschel's telescope at a distance of 3-375 light-years. This is about the distance ascribed to the I9I2-] DEPTH OF THE MILKY WAY. 6 remoter stars of the Alilky Way by Newcomb and many other modern writers ; but of course it is much too small, for the follow- ing reasons : (a) Newcomb and other astronomers cite the possibility of some of the stars being as much as 1,000,000 times brighter than the average solar star, and in that case the star might be seen at V 1,000,000= 1,000 times that distance, or 3,375,000 light-years, with an instrument having a space penetrating power no greater than that employed by Herschel, provided that no light is extinguished in its passage through space. (b) If the telescope be more powerful than Herschel's 20-foot reflector, the light gathered will be increased in the ratio of .i'-/(i8)", where .x- = diameter of mirror; and for the 60-inch reflector at Pasadena, .r=^6o, over nine times as much light could be gathered, or stars seen over three times as far away. Thus if the stars have only about 10,000 times the luminosity of the sun, they could still be seen with the Pasadena reflector at a distance of over a million light-years. For 3,375 l.-y. X 3 X 100=1,012,500 light-years. (c) The sensitiveness and accumulative effects of the photo- graphic plate, will enable us to extend our sounding line still further out into space by some three magnitudes, or four times the distance ; and thus with a modern 60-incli reflector we could photograph stars at a distance of about four million light-years, if they have 10,000 times the standard solar luminosity, and no light is lost in space. How much light is really lost in space will be considered later, but it may be stated here that it probably is decidedly less than was con- cluded by Struve. § 3. Independent Calculation of the Distance of the Remotest Stars of the Helium Type. From the data given in Lick Observatory Bulletin No. 195, we find that 225 helium stars employed by Campbell in his line of sight work have an average visual magnitude of 4.14. Of the four variables given in this Bulletin, we have used the maximum bright- ness in three cases, because they are of the algol type. In the case 6 SEE— DETERMINATION OF THE [Januarys. of ullerculis, \vc have used the mean magnitude, because the type of variable does not appear to be as yet well established. Here then we have 225 helium stars at an average distance of about 540 light-years. For in Lick Observatory Bulletin No. 195, p. 121, Campbell finds the 180 class B, or helium, stars to have an average distance of 543 light-years, while in Publications of the Astronomical Society of the Pacific for June-August, 191 1, p. 159, Professor Curtis gives 534 light-years as the average distance of 312 helium stars. The former distance for 180 stars being greater than the latter distance for 312 stars, we may take 540 light-years as the distance of the 225 helium stars here under discussion, the average magnitude of which is 4.14. If the average magnitude were decreased to 21.14, by removal to 2,512 times their present distance, which would reduce the average brightness by 17 magnitudes, the distance of the stars would be multiplied by 2,512, and become 1,356,480 light years. This is for the helium stars as they are, without any hypothesis as to bright- ness, or as to the extinction of light in space, which will be con- sidered later. The question will naturally be asked whether helium stars really exist at these great distances. We may unhesitatingly affirm that they do, because of the well-known whiteness of the small stars of the Milky Way. It is true that Pickering has investigated the dis- tribution of the helium stars in the Harvard Annals, \o\. 56, No. II., and Campbell quotes these data in Lick Observatory Bulletin No. 195 as showing that the helium stars are all bright objects. Pickering believed his tabulations to indicate " that of the bright stars, one out of four belongs to this class (B), while of the stars of the sixth magnitude there is only one out of twenty; and that few if any would be found fainter than the seventh or eighth magni- tude." The implication here is that no helium stars exist at very great distances corresponding to small magnitudes; but of course such a" view is untenable. It probably is true that the group of helium stars at a distance of some 540 light-years from our sun, and thus comparatively near 1912.] DEPTH OF THE MILKY WAY. 7 us, does cease after a certain faintness and distance has been reached; but is equally certain that other clusters or clouds of helium stars recur at greater distances, among the millions of small white stars constituting the Milky Way. For as Herschel long ago noticed the Galaxy is everywhere observed to traverse the circuit of the heavens in a clustering stream; and our view of it from the region of the sun is not essentially different from the view that could be obtained from other points in this starry stratum. Add to this consideration the fact of the well-known whiteness of the small stars in the Milky Way, and we are authorized to conclude that an indefinite number of clusters or groups of helium stars will be found in the Milky Way, and thus such stars will certainly exist at the greatest depths to which our giant telescopes can penetrate. We must therefore be on our guard against the superficial view, that because the helium stars near the sun fade away as the sixth magnitude is approached, other groups of stars of this type do not occur at greater distances. The typical whiteness of the millions of small stars which make up the Milky Way, and the clustering character of that magnificent collection of stars, alike forbid any such inference. Herschel had the correct view of the constitution of the Galaxy a century ago. Unfortunately his works have been very inaccessible, and are so little used that many erroneous conceptions have been given currency by more superficial investigators. It is impossible to commend too highly the movement now on foot in England to reissue the collected works of Sir William Herschel. In all that pertains to the sidereal universe as a whole he is easily the greatest of all modern astronomers, and will always remain unrivaled. § 4. Explanation of the Methods Employed by Campbell for Finding the Average Distance of the Group of Naked Eye Helium Stars. This is essentially a combination of the line of sight motion as found at Lick Observatory, with the proper motions resulting from observations with the meridian circle, by many observers, as worked 8 SEE— DETERMINATION OF THE [January 5, lip by Boss of the Dudley Observatory, Albany, New York. By the recent study of several thousand of the brighter stars included in his Preliminary General Catalogue, Professor Boss has deduced their proper motions with a high degree of accuracy. Campbell found from i8o of these stars resembling our sun in spectral type that their average cross proper motion in the sky, from the values derived by Boss, was about o.ii second of arc per annum, while at the same time their average speed in the line of sight shown by the spectrograph at Lick Observatory was 8.9 miles per second, or two hundred and eighty million miles a year. Having the average motion in the line of sight, in absolute units, and the average cross proper motion in seconds of arc, it is easy to find how far away a base line of 280 million miles would have to be to subtend an angle of O.II of a second of arc. It turns out to be ninety-two light-years. In this way it is possible to get the average distances of large groups of stars. Here are some of the results found by Campbell. Average Yearly Average Radial Average Rela- Average Dis- Type. No. Cross-motion. Velocity in Miles per Second. tive Parallax. tance in Light- years. B-B, 312 o!oo78 3-9 0.0061 534 Bs-Bg 90 0.0182 4.2 0.0129 253 A 172 0.0368 6.5 0.0166 196 F 180 0. I07S 8.9 0.0354 92 G 118 0.0748 9-9 0.0223 146 K 346 0.0516 10 4 0.0146 223 M 71 0.0384 10.6 0.0106 308 This table contains the most important results of the Campbell- Boss method of obtaining average distances for large groups of stars. It need scarcely be remarked that its significance can hardly be overrated. But whilst the average values given are quite trust- worthy, the method is of course inapplicable to the individual stars; and if their distances are to be found recourse would have to be had to the standard method of paralla.xes, or to the spectroscopic method in the case of visual binaries. I9I2.] DEPTH OF THE MILKY WAY. 9 § 5. Some of the Distances of the Remotest Stars as Heretofore Calculated by Astronomers. 1. Sir William Herschel, Phil. Trans. ^ 1802, p. 498, " almost 2,000,003 light- years." 2. Sir John Herschel, " Outlines," edition of 1869, p. 583, " upwards of 2,000 light-years." 3. Guillemin, " The Heavens," trans, by Lockyer, 1867, p. 433, " upwards of 20,000 light-years." 4. Bartlett, " Spherical Astronomy," 1874, p. 149, " upwards of 2,437.5 light- years." 5. Newcomb, " Popular Astronomy," edition of 1878, p. 481, " about 14,000 light-years" (for the Herschel stars). 6. Gierke, " System of the Stars," 1890, p. 314, "less than 36.000 light-years." 7. Ranyard, " Old and New Astronomy," 1892, p. 748, " less than 70,000 light- years." 8. Young, " General Astronomy," edition of 1904, p. 563, " 10,000 to 20,000 light-years." 9. Newcomb, " The Stars," 1908, p. 319, " at least 3,000 light-years." 10. See, " Researches," Vol. H., 1910, p. 638, " 4,500,000 light-years." From this table it will be seen that there was a great falling off in the distances following the epoch of Sir William Herschel; and that the present writer was the first to recognize the fallacy of the recent estimates of distance, and to restore the large values used by that unrivaled astronomer one hundred and ten years ago. Here we have a good illustration of the retrogradation of opinion in astron- omy, under the cultivation of inferior genius. Sir John Herschel's preference for such small distances over the large values used by his father is indeed remarkable and very regrettable. Evidently the small value used by Newcomb is simply an echo of the reduction in distance made by Sir John Herschel. The absurdity of these small values — not over five times that of the helium stars of 4.14 magni- tude investigated at Lick Observatory — ought to impress us with the small importance to be attached to any opinion merely because it is currently accepted. Thus we have a clear case of misleading tra- dition transmitted from the second Herschel, and the amazing spec- tacle of the whole world using values about a thousand times too small, for the greater part of a century, in times which were sup- posed to be very enlightened ! Strange indeed that the correct work 10 SEE— DETERMINATION OF THE [Januarys. of the great Sir William Herschel should have been neglected all this time! Will it seem credible to future ages that such a remark- able retrogradation of opinion could have occurred and persisted during the nineteenth and twentieth centuries? If so, it must be attributed to the narrowing effects of extreme specialization, which, with the advance of science, has been difificult to avoid in our time, and yet is utterly disastrous to the growth of true natural philosophy as the study of nature in the widest sense. §6. Other Methods for Confirming the Great Depth OF the Milky Way. (a) The girdle of helium stars about our sun, according to the Lick determination, has a mean distance of 540 light-years, or a mean diameter of 1,080 light-years. If this be one twentieth of the average thickness of the Milky Way stratum, as one may infer from the appearance of certain clusters in the constellation Sagittarius, which are near enough to be studied intelligently, then we have 21,600 light-years for the average thickness of the ]\Iilky Way. Now when we traverse the Milky Way from Centaurus to Cepheus, over an arc of 180° in length, the central band appears to the naked eye to have a width of 3° or 4°, as was long ago remarked also by Herschel and Struve. This is an extension along the circle of the Galaxy of about 60 times its thickness. If then the thickness be 21,600 light-years, the double depth of the stratum in both directions becomes about two thirds of 21,600 X 60=864,000 light-years. And if only the faint or distant telescopic stars be considered, the width of their belt of distribution is narrower, and the depth would be found several times greater yet. Wherefore it seems certain that the profundity of the Milky Way, considerably exceeds a million light-years, and may be several times that depth. (b) Accordingly if we make the very moderate hypothesis that the width of 3° or 4°, which was also noticed by Herschel and Struve, represents chiefly the nearer portion of the Galaxy; and that the remoter portion has a width not exceeding 1°, we should conclude that the depth may be found by multiplying the thickness I9I2.] DEPTH OF THE MILKY WAY. 11 or apparent angular width of 21,600 light-years by the number of degrees in the radius, 57.3. This gives for the depth 1,237,680 light- years, and this value might be considerably increased by adjustments in the data which are not improbable. (c) In addition to these general arguments, founded on the prin- ciples of geometry, we might introduce another based on actual measurement. The Lick helium stars, of average brightness 4.14 mag., were found to have an average distance of 540 light-years. If they were brought near enough to us to appear of ist magnitude, this distance would have to be divided by 4= V (2.512)^, and thus we find for the first magnitude helium stars a distance of 135 light-years. Now in calculating the plan of the construction of the heavens, from the apparent breadth of the Milky Way, Herschel arrived at the conclusion that the thickness of the stratum is about 80 times greater than the diameter of the sphere including the first magnitude stars represented by Sirius (Phil. Trans., 1785, p. 254). And if the average distance of these stars be taken as 135 light-years, the mean diameter of the shell in which they are included will be 270 light- years. This would give exactly 21,600 light-years for the thickness of the stratum of the Milky Way, as before. It is true that Herschel classed all first magnitude stars in one group, and took no account of the fact that the helium stars are the more remote and the more brilliant ; yet regarding the Galaxy as a stratum of stars chiefly of the helium type, which certainly is true of all the more distant portions of that magnificent collection of stars, we may consider the reasoning of this great astronomer as still valid. And the argument in regard to the depth of the IMilky Way is thus the same as that given above under (a) and (b). m § 7. The Effects of the Extinction of Light in Space. This problem has been treated with some detail in the 23d chap- ter of my "Researches," Vol. II., 1910, but we shall here examine the subject with greater care, especially as to the most probable average value of the coefficient of extinction. The light was shown 1'2 SEE— DETERMINATION OF THE [January 5, by Struve to be defined by the equation (0.990651 )--S (I) where x is the distance of the star, in units of A= \/(2.5i2)" and n is the diflference in magnitude. At very great distances nearly all the light is cut off, and it therefore becomes a question of high importance to determine as accurately as possible the proper value for the coefficient of extinction. Struve's value, used in the above formula, seems to be too large, and I have therefore calculated a new table, to show the effect of decreasing the coefficient. In justification of this course it should be recalled that Sir William Herschel ignored extinction entirely; but while this procedure obviously is defective, it is pretty clear, from the aspects of the Alilky Way as now made known by modern research, that Struve's coefficient is decidedly too large. The follow- ing table shows the effects of varying the coefficient, upon stars 17 magnitudes fainter, corresponding to a distance 2,512 times larger, where x — 1=2,511. Table for Varying Coefficient of Extinction. A = Coefr. of Extinction. A^-i. Fractional Part of Light IVansmitted, in Spite of Extinction. 0.99065 I 0-995 0.996 0.997 0.998 0.999 0-9995 I .ocobo 0.000,000,000,05709 0.000,003,4072 0.000,042,571 0.000,52923 0.006,5567 0.081,091 0.284,846 1.000,00 17514OOOOOO ^ ' I 293 490 I 23490 I 1889.5 I 152.51 {.See's value) 12.332 ^ I 3-5 '07 i.oooco (Herschel's value) From the study of this table, we perceive that at the distance I912-] . DEPTH OF THE MILKY WAY. 13 .t- = 2,512, corresponding to an enfeeblement of 17 magnitudes, from mere increase of distance alone, the extinction of light varies from almost total loss, with Struve's coefficient, to no loss whatever, on Herschel's tacit hypothesis of zero extinction. This latter view, however, certainly is extreme, and probably all modern astronomers agree that there is extinction of light due to cosmical dust in space. A hazy background of dust is shown on the photographs of the Milky Way and other portions of the sky, and proved to pervade the solar system by the universal prevalence of meteors. Since, however, both comets and nebulae are found to be extremely tenuous bodies, and observed to transmit the light of stars with but excessively slight enfeeblement, it is obvious that the general extinc- tion will be much smaller still, but yet appreciable. I have therefore adopted a coefficient of 0.999, about one hundredth larger than Struve's, as best harmonizing all known phenomena. This value, it is true, is much nearer to Herschel's than to Struve's coefficient, yet it admits an extinction of light which becomes appreciable at great distances, while for moderate distances it is nearly insensible ; and I believe this to correspond closely with all the known facts of the sidereal universe. An enfeeblement of one twelfth at a distance appropriate to stars 17 magnitudes fainter, could easily be compensated for by a corresponding abnormal brilliancy of the remotest stars, which on several grounds seems to be highly probable. Thus our procedure involves no extravagant assumptions as to the great brightness of the most distant stars, or as to large extinction of light, while on the other hand it avoids Herschel's tacit hypothesis of zero extinction, which certainly is unjustifiable.^ ^ In an important paper read to the Bavarian Academy of Sciences, June 10, 191 1, p. 459, Professor H. von Seeliger likewise reaches the conclusion that the absorption is very small, amounting to 0.34 of a magnitude at 780 times the distance of Sirius, which Seeliger takes for the border of the sidereal system. 14 SEE— DETERMINATION OF THE [Januarys. §8. A Graphical Method for Determining the Depth of the Galaxy, Based on the Study of Clusters. 1. Make a diagram of lo or 20 concentric circles, separated by equal intervals, each corresponding to 100 million light-years. In this scheme no clusters will be included within the central circle, because the actual measurements for parallax have excluded this possiljility. P>ut the various clusters of the N.G.C. may be plotted within the outer circles, or beyond them all, according to the results given by Herschel's rule of brightness. 2. It is required therefore to locate the clusters, and to indicate their apparent angular diameters by dots of appropriate size. Some allowance must of course be made for the varying stages of develop- ment of the different clusters, but if there is a decreasing angular diameter with distance it may be held that the method of estimating distance devised by Herschel is essentially valid, and in fact our only method of fathoming these immense distances, and thus deter- mining the depth or profundity of the Milky Way. 3. A careful attempt has been made to apply this method, using the data of the N.G.C, and the results of the Crossley photographs recently obtained at Lick Observatory. The results of this investi- gation are shown to confirm the present theory. §9. Final Test of the Indefinite Extension of the ]\IiLKY Way Desirable. This should be made by the graphical method just outlined, but by means of more powerful instruments than any yet systematically employed in this work. To feel satisfied that the universe extends on indefinitely, we must have proof of additional clusters of stars of smaller magnitude, and more compressed constitution, as from the narrowing effect of perspective, at great distances. Probably we shall not know what the sidereal heavens contain in the way of vanishing clusters till the Milky Way is systematically photographed for just such objects, and this very likely will require a long cam- paign of photographic research with a large instrument. But as many large reflectors are now coming into use, we may hope for it I912-] DEPTH OF THE MILKY WAY. 15 before many years elapse. This would be completing on a modern scale the sidereal soundings left somewhat incomplete by the sys- tematic explorations of the Herschels. In a private letter, written in response to my recent inquiry re- garding the power of the 6o-inch reflector of the Solar Observatory at Mt. Wilson, Professor W. S. Adams, the Acting Director, informs me that this fine instrument probably will show visually stars as faint as 1 8th magnitude. He points out, however, that the magnitude scale is not well defined for such faint objects, and that very few astronomers have enough experience to fix it at the present time. Adams also informs me that from a photograph of the region of the northern celestial pole of four hours' duration. Professor E. C. Pickering has derived a value of 21.0 magnitude for the faint- est stars, by the system of photographic magnitudes in use at the Harvard College Observatory. Obviously there is some uncertainty in this value, but it probably is not extreme. In answer to an inquiry as to the possibility of getting still fainter stars by prolonging the exposure, Professor Adams assures me that it can be easily done, the only limit being the brightness of the background of the sky; but that with the clear air of Mt. Wilson this would not be reached till the exposure had extended over many hours. He adds that it takes about three times the exposure to obtain a star one magnitude fainter. From the data here supplied it seems certain that stars as faint as 21.0 magnitude may be photo- graphed at Mt. Wilson, with the 60-inch reflector, and that by pro- longing the exposure several additional hours or through whole nights, stars of 22.0 magnitude probably could be obtained. It is therefore well established that stars 17 magnitudes fainter than the 225 helium stars, with average magnitude of 4.14, recently investigated at Lick Observatory, may now be photographed with more than one instrument; and the value of A = 2,5 12 used in our calculations is amply justified. In fact it seems probable that instead of 2,512 as our distance multiplier for stars 17 magnitudes fainter, we might have used the larger value 3,981, corresponding to stars 18 magnitudes fainter than our 225 helium stars with average magni- 10 SEE— DETERMINATION OF THE [Januarys. tude of 4.14. This would almost have doubled the calculated depths of the Milky Way throughout the foregoing discussion, and given us over two million light-years, exceeding the profundity originally concluded by Ilerschel in 1802. In the Phil. Trans, for 1800, pp. 83-4, Herschel finds by a different process that a cluster of 5,000 stars visible in his 40- foot telescope is distant 11,765,475,948,678,- 678,679 miles, " a number which exceeds the distance of the nearest fixed star at least three hundred thousand times." With modern data this proves to be 460,355 times the distance of Alpha Centauri, or 2,001,120 light-years. § 10. Summary of the Chief Results of the Determination OF THE Depth of the Milky Way. From the several independent and mutually confirmatory argu- ments here adduced it follows that the depth of the Milky Way decidedly exceeds a million light-years, and substantially accords with the profundity concluded by the illustrious Herschel one hun- dred and ten years ago. 1. Herschel concluded that with his forty-foot reflector he per- ceived stars whose light had occupied two million years in reaching the earth; and he justly remarked that he had seen further into space than any human being before him. The visual power or light grasp of Herschel's telescope is somewhat surpassed by modern instruments; and much additional power is given to the modern instrument by the use of photography. 2. But if, on the one hand, the modern instruments surpass Herschel's in power, there is on the other some increased need for this in that we now attempt to take account of the extinction of light by cosmical dust in space. Neglecting this loss of light, Herschel may have slightly overestimated the distances to which his telescope could penetrate, but the error was scarcely of sensible importance. 3. With our greatest modern instruments and the use of pho- tography it is certain that we can observe stars- at a distance of over *In Astron Nachr., No. 4.536, Nov. 13, 1911, Professor F. W. Very con- cludes that the White Nebula may be galaxies at a distance of a million light- I912-] DEPTH OF THE MILKY WAY. 17 two million light-years, and it is very probable that we can penetrate to a depth of about five million light-years. A modern silver-on- glass reflector of twelve feet aperture would give about six times as much light as the 6o-inch reflector at Pasadena, and with this gain of two magnitudes in light power it is probable that we could penetrate into space at least twice this distance (theoretically 2.512 is the factor) or to a depth from which the light zuould take ten million years to reach the earth. At the present time a 12-foot reflector is possible, and the depth to which we can penetrate is simply a question of telescopic power, which can be vastly but not indefinitely increased. And this is true in spite of the extinction of light by cosmical dust in space. There is a limit to the distance to which any given telescope can penetrate, but it increases steadily with the aperture, since the only question involved is one of enormous light grasp. It is to be hoped that a telescope of not less than 12 feet aperture may be built for use on the Milky Way. With such a giant instru- ment discoveries of the highest order might confidently be antici- pated. A modern-- expansion of our views of the sidereal universe analogous to that which marked the great epoch of Herschel would follow, with the most beneficial effects upon every branch of astro- nomical science. Recent developments in many lines show that the epoch of great discoveries has not passed, but is in fact just begin- ning : and the estimates here laid down, as to the depth and magnifi- cent extent of the Milky Way, convey to us but a dim outline of the discoveries which await the builders of the giant telescopes of the future. In this great advance America may naturally be expected to take the leading part. Starlight, on Loutre, Montgomery City, Missouri, November 4, 191 1. years. The view adopted in my " Researches," Vol. II., 1910, however, is much more probable, since it gives continuity to the various types of bodies observed to constitute the sidereal universe. Note added Dec. 16, 1911. PROG. AMER. PHIL. SOC, LI. 203 B, PRINTED MARCH 16, I9I2. CONTRABAND OF WAR. By John Bassett Moore. (Read February 2, 1912.) The word contraband (Italian, contrahbando; Spanish, contra- band 0) signifies something prohibited — a trade carried on, or an article imported or dealt in, in violation of some inhibition. Thus, smuggled goods are often spoken of as contraband. The term contraband of war denotes commodities which it is unlawful to carry to the country, or to the military or naval forces, of a belligerent. By a " belligerent " is meant one of the parties to a war. Often the word "enemy" is used instead of "belligerent." Writers constantly speak of an " enemy " or " enemy's " country, an " enemy " ship, or " enemy " goods, meaning thereby merely that the country, or the ship, or the merchandise, is that of a party to a war, that is to say, of a belligerent government or of one of its citizens. Sometimes the word "/zo.y///^" is used instead of "enemy." When war breaks out between two countries, the carrying on of trade by the citizens of the one country with those of the other becomes unlawful; but the same general interruption does not extend to the commercial intercourse between the parties to the war and third parties, called neutrals. The intercourse between the bel- ligerents and neutrals continues. This continuance is regarded not as a favor granted to the belligerents but as a right belonging to neutrals. As between the belhgerents, neither is required to grant to the other any privilege in respect of trade. On the contrary, they endeavor to subdue each other by attacks upon persons and upon property. This is their acknowledged right. But the rest of the world, composed of neutral powers, having no part in the quarrel and perhaps little concern in the issue, also has its rights. Its interests and convenience are not to be wholly subordinated and sacrificed to the exigencies of the one or the other of the belligerents, 18 1912] MOORE— CONTRABAND OF WAR. ]9 each of whom, while desirous to preserve its own trade, would of course be glad to cut off altogether that of its enemy; and it is there- fore acknowledged to be the right of neutrals to continue their com- merce with the belligerents, subject only to the restrictions imposed by the law of contraband and of blockade. In proceeding to the discussion of the particular subject of con- traband, it is proper to advert to the confusion which seems so widely to prevail as to the legal position of the prohibited trade. The statement is frequently made that the trade in contraband of war' is lawful, even though this broad affirmation be immediately followed by the admission that the trade is carried on subject to the risk of capture and confiscation of the goods, and of the deten- tion, loss of freight and perhaps even the confiscation of the ship. This admission should alone suffice to put us on our guard. Mer- chandise is not confiscated, voyages are not broken up, ships are not condemned, for acts that are innocent ; these severe and destructive inflictions are penalties imposed for acts that are unlawful. The confusion so often exhibited on this subject is due to the neglect of certain simple but fundamental truths, namely, that, in the inter- national sphere, and particularly in matters of neutrality, the cri- terion of lawfulness is primarily furnished by international law and not by municipal law, lawfulness according to the latter by no means implying lawfulness according to the former; that, between the acts which neutral governments and their citizens are forbidden to com- mit and the acts which neutral governments are obliged to prevent, there is a wide distinction; that, by international law, acts that are unneutral in the sense of being unlawful are, from the point of view of their prevention and punishment, divided into two classes, (i) those which neutral governments are bound to prevent and punish, and (2) those which neutral governments are not bound to prevent and punish ; that municipal law is supposed to prohibit, not all the unneutral acts which international law forbids, but only that part of them which neutral governments are bound to repress, the pre- vention and punishment of the rest being left to the belligerents as the parties primarily interested. Obviously, the determination of the question whether an act is lawful or unlawful depends not upon 20 MOORE— CONTRABAND OF WAR. [Februarys, the circumstance that the right or duty to punish it is committed to one agency or another, but upon tiie fact that it is or is not punish- able. Tlie proof that it is unlawful is found in the fact that its com- mission is penalized. All acts for the commission of which inter- national law prescribes a penalty are in the sense of that law unlaw- ful. That there are various acts of this kind, such as the supplying of contraband of war to a belligerent, which neutrals are not obliged to prohibit and punish by their municipal law, merely signifies that the interests of neutrals have not been regarded as negligible, and that there are limits to the burdens which they have been required to assume and to the exertions which they are required to make. Should a neutral government itself supply contraband of war to a belligerent it would clearly depart from its position of neu- tralitv. The private citizen undertakes the business at his own risk, and against this risk his government can not assure him protection without making itself a party to his unneutral act. These propositions are abundantly established by authority. Maritime states, says Hefifter, have adopted, in a common and reciprocal interest, the rule that belligerents have the right to restrict the freedom of neutral commerce so far as concerns contraband of war, and to punish violations of the law in that regard. . . . This right has never been seriously denied to belligerents.* Says Kent : The principal restriction which the law of nations imposes on the trade of neutrals is the prohibition to furnish the belligerent parties with warlike stores and other articles which are directly au.xiliary to warlike purposes.* Says Woolsey : If the neutral [government J should send powder or balls, cannon or rifles, this would be a direct encouragement of the war, and so a departure from the neutral position. . . . Now, the same wrong is committed when a private trader, without the privity of his government, furnishes the means of war to either of the warring parties. It may be made a question whether such conduct on the part of the private citizen ought not to be prevented by his government, even as enlistments for foreign armies on neutral soil are. made penal. But it is diflicult for a government to watch narrowly the operations of trade, and it is annoying for the innocent trader. Moreover, * Hefftcr, " Droit Int.," Bergson's ed., by GefFcken, 1883, p. 384. 'Kent, "Int. Law," 2d ed., by Abdy, 330. I9I5.] MOORE— CONTRABAND OF WAR. 21 the neutral ought not to be subjected by the quarrels of others to additional care and expense. Hence by the practice of nations he is passive in regard to violations of the rules concerning contraband, blockade, and the like, and leaves the police of the sea and the punishing or reprisal power in the hands of those who are most interested, the limits being fixed for the punishment by common usage or law. ... It is admitted that the act of carrying to the enemy articles directly useful in war is a wrong, for which the injured party may punish the neutral taken in the act.^ Says Manning: The right of belligerents to prevent neutrals from carrying to an enemy articles that may serve him in the direct prosecution of his hostile purposes has been acknowledged by all authorities, and is obvious to plain reason. . . . The nonrecognition of this right . . . would place" it in the power of neutrals to interfere directly in the issue of wars — those who, by definition, are not parties in the contest thus receiving a power to injure a belligerent, which even if direct enemies they would not possess.* Says Creasy : A belligerent has by international law a right to seize at sea, and to appro- priate or destroy, articles, to whomsoever they may belong, which are calcu- lated to aid the belligerent's enemy in the war, and which are being conveyed by sea to that enemy's territory.^ Says Holland : The neutral power is under no obligation to prevent its subjects from engaging in the running of blockades, in shipping or carrying contraband, or in carrying troops or dispatches from one of the belligerents ; but, on the other hand, neutral subjects so engaged can expect no protection from their own government against such customary penalties as may be imposed upon their conduct by the belligerent who is aggrieved by it." The fact that the supplying of contraband of war is considered as a participation in the hostilities is shown not only by the authority of writers, but also by numerous state papers. Washington, in his famous neutrality proclamation of April 22, 1793, countersigned by Jefferson, as Secretary of State, announced that whosoever of the citizens of the United States shall render himself liable to punishment or forfeiture under the law of nations, by committing, aiding, or abetting hostilities against any of the said powers, or by carrying 'Woolsey, "Int. Law," §§178, 179- * Manning's " Law of Nations," Amos's edition, 352. ° Creasy, " First Platform of Int. Law," 604. ° Holland, "Studies in Int. Law," 124-125. See, also, Moore, Digest of Int. Laiv, VII., 9/2-973- 22 MOORE— CONTRABAND OF WAR. [Februarys, to any of them those articles which are deemed contraband by the modern usage of nations, will not receive the protection of the United States against such punishment or forfeiture.'' Jefferson, in his subseqtient note to the British minister, May 15, 1793, observes that in the case of contraband the law of nations is satisfied with the "external penalty" pronouncecd in the Presi- dent's proclamation.^ President Grant, in the proclamation issued by him August 22, 1870, during the Franco-German war, declares, in the most precise terms : While all persons may lawfully, and without restriction, by reason of the aforesaid state of war, manufacture and sell within the United States arms and munitions of war, and other articles ordinarily known as " contra- band of war," yet they can not carry such articles upon the high seas for the use or service of either belligerent, . . . without incurring the risk of hostile capture and the penalties denounced by the law of nations in that behalf. And I do hereby give notice that all citizens of the United States, and others who may claim the protection of this Government who may misconduct them- selves in the premises, will do so at their peril, and that they can in no wise obtain any protection from the Government of the United States against the consequences of their misconduct.* In the neutrality proclamations, issued during the war between the United States and Spain, the following provisions are found, in which the furnishing of arms and munitions of war to either party to the conflict is expressly treated as an act of unneutrality. The Brazilian government, by a circular of April 29, 1898, de- clared to be " absolutely prohibited " the " exportation of material of war from the ports of Brazil to those of either of the belligerent powers, under the Brazilian flag or that of any other nation."^*' The King of Denmark issued April 29, 1898, a proclamation prohibiting Danish subjects "to transport contraband of war for any of the belligerent powers. "^^ Great Britain's proclamation of April 23, 1898, warned British subjects against doing any act " in derogation of their duty as sub- ' Am. State Papers, For. Rel., I., 140. * Moore, "Digest of Int. Law," VII., 955. "Moore, "Digest of Int. Law," VII., 75i- ^° Proclamations and Decrees during the War with Spain, 13. " Proclamations, etc., 22. 1912.] MOORE— CONTRABAND OF WAR. 23 jects of a neutral power," or " in violation or contravention of the law of nations," among which was enumerated the carrying of " arms, ammunition, military stores or materials " ; and declared that "all persons so offending, together with their ships and goods, will rightfully incur and be justly liable to hostile capture, and to the penalties denounced by the law of nations. "^- The governor of Curagao, acting under instructions of the min- ister of the colonies of the Netherlands, issued a decree prohibiting " the exportation of arms, ammunition, or other war materials to the belligerents."^^ Portugal, while stating, in Article IV. of her neutrality decree of April 29, 1898, that "all articles of lawful commerce" belonging to subjects of the belligerent powers might be carried under the Por- tuguese flag, and that such articles belonging to Portuguese subjects might be carried under the flag of either belligerent, yet declared: " Articles that may be considered as contraband of war are expressly excluded from the provisions of this article."^* Were further proof needed of the unneutral and noxious char- acter of contraband trade, it might be found in the doctrine of infec- tion, under which innocent cargo is condemned when associated with contraband merchandise of the same proprietor, and the transporta- tion penalized by loss of freight and expenses, and, under various circumstances, by confiscation of the ship. Bearing in mind that the subject which we are considering is one of universal interest, directly affecting the world's trade and involving the imposition of heavy pecuniary penalties upon indi- viduals, one ventures little in saying that among present-day ques- tions of maritime law, touching intercourse between belligerents and neutrals, the most important is that of contraband. This may be affirmed in spite of the fact that, partly because of the lack of great maritime wars in recent times, its gravity may not at the moment be generally or popularly appreciated. The question of "Id., 35. "Id., 27. " Id., 61. See, also, the proclamation of the taotai of Shanghai, id., 20, and the instructions of the Haitian Government, id., 39. 24 MOORE— CONTRABAND OF WAR. [Februarys, blockade, although it once assumed immense proportions, to a great extent lost its importance when the principle was established that blockades in order to be legally valid must be effective, that is to say, maintained by a force sufficient to prevent access to the block- aded port or at least to render such access dangerous. Since the definite and universal acceptance of this principle, by which neutral commerce was relieved of the hazards to which it was formerly exposed from measures generically designated by the evil name of " paper blockades," the conflict between belligerent right and neutral right has been carried on chiefly in the domain of contraband, to which it may be said that all the legal uncertainties that formerly attended the subject of blockade have been transferred, with many additions and aggravations. In order to demonstrate the paramount importance of the ques- tion of contraband, it is unnecessary to do more than point out that, if the claim of capture on this ground be not properly limited, the two great safeguards of neutral rights established after generations of conflict become utterly worthless. I refer to the rule that free ships make free goods and the rule that blockades must be effect- ively maintained. First, let us consider the rule that free ships make free goods. By what has been called the common law of the sea, the goods of an enemy were subject to capture and confiscation without regard to the character of the ship in which they were borne. The enforce- ment of this rule necessarily involved the capture and bringing in of neutral vessels whose cargoes were alleged to be composed even in small part of the goods of a belligerent. The breaking up of the voyages of neutral vessels in this manner, with all the resultant losses, involved so much hardship to carriers in no way concerned in the conflict that, as early as the seventeenth century, there sprang up an agitation for the exemption of neutral vessels from molesta- tion for carrying goods which happened to belong to a citizen of a belligerent country. Such an exemption gradually came to be em- bodied in treaties; and when on February 28, 1780, the Empress Catherine of Russia issued her celebrated manifesto, which formed the basis of the Armed Neutrality, she announced this principle: I9I2.] MOORE— CONTRABAND OF WAR. 25 2. Goods belonging to the subjects of the said nations at war are, with the exception of contraband articles, free [from capture] on board neutral vessels. This definite enunciation of the rule that free ships make free goods was incorporated in the Declaration of Paris of 1856 in the following term : 2. The neutral flag covers the enem3''s goods, with the exception of con- traband of war. The United States, Spain and Mexico (Mexico acting under the direct influence of the United States) did not adhere to the Declara- tion of Paris, because it undertook to abolish privateering; but the United States and Spain expressly accepted the rule that free ships make free goods, and this was proclaimed by the United States in 1898 as a principle of international law and was so accepted by Spain in the war between the two countries in that year. More- over, Spain has since adhered to the Declaration of Paris in its entirety. But, note the exception to the rule. Enemy's goods are exempt from capture under the neutral flag, " with the exception of contraband of war." In other words, the operation of this rule and the protection intended to be afforded by it are wholly dependent upon the definition of contraband. Make the list of contraband long enough, and the rule becomes a farce. Secondly, take the present law of blockade. At one time ficti- tious blockades were the bane of neutral commerce. In the twelve years that followed the breach of the Peace of Amiens — the days of the so-called Napoleonic wars — millions upon millions of neutral property were unlawfully confiscated for the alleged violation of or attempt to violate blockades which existed only on paper. The declaration of the Empress Catherine above referred to con- tained the following rule : 4. To determine what constitutes a blockaded port, this denomination is confined to those the entrance into which is manifestly rendered dangerous in consequence of the dispositions made by the attacking power with ships stationed sufficiently near. The Declaration of Paris of 1856 provided: 4. Blockades, in order to be binding, must be eflfective ; that is to say, maintained by a force sufficient really to prevent access to the coast of the enemy. 26 MOORE— CONTRABAND OF WAR. [Februarys, The world accepted this principle with joyful unanimity. We may, however, pertinently inquire, What is it worth, if the definition of contraband be not properly limited ? The answer is not difficult. If the definition of contraband be so extended as to emj^race in some form, positively or conditionally, practically all articles of com- merce, the question of blockade ceases to be important. The security intended to be afforded to the neutral, by requiring the bel- ligerent to make his blockade effective, becomes a mockery ; the belligerent is practically relieved of the burden of maintaining block- ades, for, instead of keeping his ships at certain points and hamper- ing his offensive use of them, he can roam the seas at will and seize all articles destined to any belligerent port under the claim of contraband. Let us consider the significance of the question of contraband in yet another relation. It is creditable to our humanity that proposals having a benevolent sound usually evoke a prompt and generous response, but it sometimes happens that the substance upon exami- nation turns out to be less benevolent than the sound. We have lately heard much of the proposed immunity of private property at sea from capture. The United States is said to have advocated such a measure at both Hague Conferences. What has happened is actually this : Some of our earlier statesmen, notably Franklin, did in reality advocate a very wide exemption not only of property but also of persons, on land as well as on the sea, from the opera- tions of war ; and their example was followed by some of their suc- cessors. In 1857 the government of the United States, being em- barrassed by its refusal to accede to the Declaration of Paris on account of the clause abolishing privateering, offered to adhere on condition that the powers go farther and exempt private property at sea from capture; but this off'er was expressly subject to the exceptions of contraband and blockade. In 1907 Mr. Choate, on behalf of the Delegation of the United States, submitted to the second Peace Conferences at The Hague the following resolution: The private property of all citizens or subjects of the signatory powers, with the exception of contraband of war, shall be exempt from capture or seizure on the sea by the armed vessels or by the mihtary forces of any of 1912.] MOORE— CONTRABAND OF WAR. 27 the said signatory powers. But nothing herein contained shall extend exemp- tion from seizure to vessels and their cargoes which may attempt to enter a port blockaded by the naval forces of any of the said powers. What therefore the United States since 1850 has proposed is, not that private property at sea shall be exempt from capture, but that it shall be so exempt, subject to the exceptions of contraband and blockade. The proposal, as thus qualified, no doubt had a sub- stantial character in 1857, since the government of the United States at that day still recalled the limitations upon contraband for which it had traditionally contended. The case was the same when, by the treaty of commerce between the United States and Italy of February 26, 1871, it was actually agreed (Article XII.) that, in the event of war between the two countries, the private property of their citizens and subjects should be exempt from capture on the high seas or elsewhere, subject to the exceptions of contraband and blockade; for the treaty then proceeded (Article XV.) precisely to limit the scope of contraband, confining it to arms and munitions of war, and declaring that those articles " and no others " should be comprehended under that denomination.^^ But at The Hague, in 1907, the importance of the exceptions was greatly enhanced by the separate presentation on the part of the United States of an ex- tremely vague and sweeping proposition on contraband of war, in which provisions appear, no doubt for the first time in American diplomacy, in the category of absolute as well as in that of condi- tional contraband.^" Taking into consideration the objects of war, opinions will necessarily differ as to the merits and value of a pro- posal to exempt enemy ships and enemy goods as such from capture, while leaving in force the law of blockade and of contraband, with- out any precise definition or limitation of the latter. Such a pro- posal holds out no advantage to neutrals, but offers to belligerents the favor of placing them on the same footing as neutrals commer- cially. And even the extent of this favor would depend upon the definition and scope of contraband. Is there not, indeed, a certain incongruity in exempting from capture such an obviously important '* Note A, infra, p. 42. '"Note B, infra, p. 43. 28 MOORE— CONTRABAND OF WAR. [Februarys, ■ auxiliary to military and naval operations as the ships of an enemy, while subjecting to seizure and confiscation the agricultural products of a neutral? The question of contraband may now be considered in its his- torical and experimental aspects. It is unnecessary for this pur- pose to enter minutely into the origin of the subject. It suffices to say that in the sixteenth and the early part of the seventeenth cen- tury, the law of contraband and of blockade both being unsettled, belligerents often assumed the right to capture all neutral ships and merchandise bound to an enemy's port, thus in effect denying the existence of any right of neutral trade as opposed to belligerent exigencies. The neutral, if he differed with the belligerent as to the necessity of the inhibition or the propriety of the capture, would resort to reprisals. The conflicts that resulted and the constant in- terruptions of trade, rendering it impossible to carry on international commerce without risk of ruinous losses, induced governments in the latter half of the seventeenth century to concert a decided change in practice. Grotius, in his De Jure Belli ac Pads (1625), perhaps recording the transition in thought, divided articles, with reference to the ques- tion of contraband, into three classes, (i) those that were of use only in war, (2) those that were of no use in war, but served only for pleasure, and (3) those that were useful both in war and in peace (i. e., things of double use, ancipitis nsus), as money, pro- visions, ships and their appurtenances. The first he held to be pro- hibited; the second, to be free. As to the third, the circumstances of the war must, he said, be considered; and if the belligerent could not protect himself unless he intercepted it, necessity would give him the right to intercept it, " but under the obligation of restitution, except there be cause to the contrary." As an example of " cause to the contrary," he instanced the case of the supplying of a besieged town or a blockaded port, when a surrender or a peace was daily expected. ^^ By a treaty between France and the Hanse Towns, signed at Paris Alay 10, 1655, contraband was confined to munitions of war, Grotius, "De Jure Belli ac Pacis," Lib. III., c. I., v, 1-3. 17 , I9I2.] MOORE— CONTRABAND OF WAR. 29 and it was expressly declared that wheat and grains of all sorts, vegetables and other things serving to sustain life, might be carried to the enemy, provided that they were not transported to towns and places actually under attack and were taken voluntarily and not under compulsion of the enemy, in which case they might be seized and retained on paying their just value. November 7, 1659, there was concluded between France and Spain the famous Treaty of the Pyrenees. Articles XII. and XIII. dealt with the subject of contraband, including therein only such things as were distinctly of warlike character, and excluding there- from wheat, corn and other grains, pulse, oils, wines, salt, and gen- erally all things useful to sustain life, unless destined to towns and places " besieged, blocked up, or surrounded. "^^ The Dutch agreed to these categories in 1662, and were soon followed by Great Britain, in treaties made with the United Prov- inces and Spain in 1667, and with France in 1677. In 1713 came the Peace of Utrecht. By the treaties concluded between France and the other powers on that occasion, the subject of contraband was definitely regulated on the most advanced lines. For example, in the treaty of commerce with Great Britain signed April II (171 3), while contraband was limited to certain enumerated articles of warlike character, the non-contraband list, which em- braced wheat, barley and other grains, pulse, tobacco, spices, salt and smoked fish, cheese and butter, beer, oils, wines, sugars, salt, " and in general all provisions which serve for the nourishment of man- kind and the sustenance of life," was extended to many other arti- cles, all of which were declared to be free except when transported to places " besieged, blocked up round about, or invested."^'' Similar stipulations were incorporated in the British-French commercial treaty signed at Versailles September 26, 1786. In the manifesto of the Empress Catherine of Russia of 1780, which formed, as heretofore stated, the basis of the Armed Neu- trality, it was declared that her Imperial Majesty adhered to Articles X. and XL of her treaty of commerce with Great Britain, and ex- ^^Note C, infra, p. 43. " Note D, infra, p. 44. 30 MOORE— CONTRABAND OF WAR. [February 2, tended their provisions to all the nations at war. This treaty was concluded June 20, 1766. With the "single exception" of certain enumerated articles, which were " accounted ammunition or military stores," it was agreed that the subjects of the one party might trans- port " all sorts of commodities " to places belonging to the enemy of the other that were not " actually blocked up, or besieged, as well by sea as by land."^** Such was the condition of things when the wars growing out of the French Revolution began. The enthusiastic devotion of the French on the one hand to the principles which they had espoused, and the frenzied resistance of monarchical governments on the other hand to what they regarded as an anarchical propagandism threat- ening thrones everywhere by force of example if not by force of arms, imparted to these struggles a peculiarly intense and lawless character. Three months after the war between France and Great Britain was declared, the National Convention, May 9, 1793, there being a scarcity of food in France, adopted a decree authorizing the seizure of vessels laden wholly or in part with provisions, which, if found to be neutral property, were to be paid for at the price which they would have fetched at the port of destination, together with an allowance for freight and for the vessel's detention. This was a claim not of contraband but of preemption. Nevertheless, the United States protested against it, and it was not uniformly enforced against American vessels. Great Britain on the other hand, wishing not only to supply her own wants but to increase the pressure on France, advanced a claim compounded of contraband and preemp- tion. By an order in council of June 8, 1793, which was commu- nicated to the Admiralty on the 28th of the same month, the com- manders of British ships of war and privateers were authorized to seize all vessels laden wholly or in part with corn ( i. c, cereals gen- erally, as wheat, barley, rye and oats, but more especially wheat), flour, or meal, bound to any port in France, or any port occupied by the armies of France, in order that such provisions might be pur- chased on behalf of the government, with an allowance to the vessel for freight, or in order that the master might be required to give '" Note E, infra, p. 44. I9I2.] MOORE— CONTRABAND OF WAR. 31 security to dispose of such cargo in a country in amity with Great Britain. The British government assumed to justify this order on the ground that by the law of nations, as laid down by the most modern writers, and particularly by Vattel, all provisions were to be considered as contraband, and as such liable to confiscation, where the depriving an enemy of them was one of the means intended to be employed for reducing him to reasonable terms of peace ; and that the actual situation of France rendered this reasoning pecu- liarly applicable, not only because the scarcity there was caused by the unusual measure of arming almost the whole laboring class of the nation, but also because the trade was to be regarded, not as a mercantile speculation of individuals, but as an immediate operation of the very persons who had declared war and were carrying it on against Great Britain. On these considerations, said the British government, the powers at war would have been perfectly justifiable if they had considered all provisions as contraband and had directed them as such to be brought in for confiscation, but they had only sought to prevent the French from being supplied with com, omit- ting all mention of other provisions, and even in respect of com, instead of confiscating the cargoes, had secured to the proprietors, if neutral, a full indemnity for any loss they might sustain. The United States on the other hand declared that the position that provisions were contraband in the case where the depriving an enemy of them was one of the means intended to be employed for reducing him to reasonable terms of peace, or in any case but that of a place actually blockaded, was entirely new ; that reason and usage had established that, when two nations went to war, those \^ho chose to live in peace retained their natural right to pursue their agriculture, manufactures, and other ordinary vocations, and to carry the produce of their industry, for exchange, to all nations, belligerent or neutral, except that they must not furnish implements of war to the belligerents or send anything to a blockaded place. Implements of war destined to a belligerent were treated as con- traband, and were subject to seizure and confiscation. Corn, flour, and meal were not, said the United States, of the class of contra- band, and consequently remained articles of free commerce. The 32 MOORE— CONTRABAND OF WAR. [Februarys, state of ar between Great Britain and r>ance furnished neither belligerent with the right to interrupt the agriculture of the United States, or the peaceable exchange of its produce with all nations. Such an act of interference tended directly to draw the United States from the state of peace in which they wished to remain. If the United States permitted corn to be sent to Great Britain and her friends, and refused it to France, such an act of partiality might lead to war with the latter power. If they withheld supplies of provisions from France, they should in like manner be bound to withhold them from her enemies also, and thus to close to them- selves all the ports of Europe where corn was in demand, or else make themselves a party to the war. This was a dilemma into which no pretext for forcing the United States could be found. Great Britain might, indeed, feel the desire of starving an enemy nation ; but she could have no right to do it at the cost of the United States, or to make the latter the instrument of it.-^ Such was the position maintained by the United States ; and when John Jay was sent on a special mission to England in 1794 to negotiate a settlement of differences, the first topic discussed in his instructions was that of the vexations inflicted on commerce under orders in council. By the treaty which he signed on Novem- ber 19, 1794, a precise enumeration was made (Article XVIII.) of the things which were admitted to be contraband, and it was stipu- lated that when cases arose in which " provisions and other articles not generally contraband " might, according to the existing law of nations, be regarded as becoming such, they should not, even though seized on that ground, be confiscated, but should be paid for at their full value, together with a reasonable mercantile profit, freight and demurrage.-^ Nor was this all. A mixed commission was estab- lished under the treaty (Article VII.) to adjudicate complaints on account of seizures. The British authorities, where they made com- pensation for cargoes of provisions, adopted as a basis the invoice price plus a mercantile profit of ten per cent. The claimants con- tended that this was inadequate. The commission allowed the net "For a full narrative of this incident and the text of the orders in council, see Moore's " History and Digest of International Arbitrations," I., 299-306. "^ Note F, infra, p. 45. 1912.] MOORE— CONTRABAND OF WAR. 33 value of the cargo at its port of destination at the time at which it probably would have arrived there, had it not been seized. The awards of the commission in the case of captured vessels laden with provisions and bound to France are estimated to have amounted to £720,000, or approximately $3,500,000.^^ The position successfully maintained by the United States in the case of Great Britain was altogether in accord with that which was reciprocally acted upon in its relations with other powers. The commercial treaty with France of 1778 — the first treaty concluded by the United States — substantially incorporated the Utrecht clause on the subject of contraband,-" as also did the later convention of 1800. A similar stipulation may be found in the treaty with Sweden of 1783, and in that with Spain of 1795. In the treaties of 1785 and 1799 the United States and Prussia went so far as to agree that even arms and munitions of war, when seized as contraband, should not be confiscated, but that the captor should pay for them if he converted them to his own use, or pay damages if he merely detained them.-^ In the treaty between the United States and Colombia of 1824 a clause on contraband was inserted which furnished the model followed by the United States with practical uniformity in its sub- sequent treaties.-*^ It is substantially reproduced in the contraband articles of the treaty with Italy of 1871. It may also be found in identical or nearly identical terms in the treaties between the United States and the following powers: Central America, 1825; Brazil, 1828; Mexico, 1831 ; Chile, 1832; Peru-Bolivia, 1836; Venezuela, 1836 and i860; Ecuador, 1839; New Granada, 1846; Salvador, 1850 and 1870; Peru, 1851 and 1870; Two Sicilies, 1855; Bolivia, 1858; Haiti, 1864; Dominican Republic, 1867. During the war with Spain, in 1898, the subject of contraband was dealt with by the United States in General Orders No. 492, which specified certain articles as " absolutely contraband " and others as " conditionally contraband." The former included arms ^ Moore, " History and Digest of International Arbitrations," I., 343-344. -* Note G, infra, p. 46. ^ Note H, infra, pp. 47-48. =" Note /, infra, p. 48. PROC. AMER. PHIL. SOC, LI. 203 C, PRINTED MARCH 16, I9I2. 34 MOORE— CONTRABAND OF WAR. [February 2, and munitions of war and machinery for their manufacture, salt- peter, military accoutrements and equipments, and horses. The " conditionally contraband " were : Coal, when destined for a naval station, a port of call, or a ship or ships of the enemy ; materials for the construction of railways or telegraphs, and money, when such materials or money are destined for tlie enemy's forces; provisions, when destined for an enemy's ship or ships, or for a place that is besieged. In the early stages of the Boer war a question arose between the United States and Great Britain as to the seizure of various articles shipped at New York, some of them on regular monthly orders, by American merchants and manufacturers on the vessels Beatrice, Maria, and Mashona, which were seized by British cruisers while on the way to Delagoa Bay. These articles consisted chiefly of flour, canned meats, and other foodstuffs, but also embraced lumber, hardware, and various miscellaneous articles, as well as quantities of lubricating oil, which were consigned partly to the Netherlands South African Railway, in the Transvaal, and partly to the Lourengo Marques Railway, a Portuguese concern. It was at first supposed that the seizures were made on the ground of contraband, and with reference to this possibility the government of the United States, on January 2, 1900, declared that it could not recognize their validity " under any belligerent right of capture of provisions and other goods shipped by American citizens in ordinary course of trade to a neutral port." It soon transpired, however, that the Beatrice and Mashona, which were British ships, and the Maria, which, though a Dutch ship, was at first supposed to be British, were arrested for violating a municipal regulation forbidding British subjects to trade with the enemy, the alleged offense consisting in the transportation of goods destined to the enemy's territory. The seizure of the cargoes was declared to be only incidental to the seizure of the ships. As to certain articles, however (particularly the oil consigned to the Netherlands South African Railway in the Transvaal), an allega- tion of enemy's property was made; but no question of contraband was raised, and it was eventually agreed that the United States consul-general at Cape Town should arrange with Sir Alfred Milner, 1912] MOORE— CONTRABAND OF WAR. 35 the British high commissioner, for the release or purchase by the British government of any American-owned goods, which, if pur- chased, were to be paid for at the price they would have brought at the port of destination at the time they would have arrived there in case the voyage had not been interrupted. In the course of the correspondence. Lord Salisbury thus defined the position of the British government on the question of contraband : Food stuffs, with a hostile destination, can be considered contraband of war only if they are supplies for the enemy's forces. It is not sufficient that they are capable of being so used; it must be shown that this was in fact their destination at the time of the seizure. This statement by Lord Salisbury was in harmony with what is laid down in Holland's Manual of Naval Prize Law, issued by the British Admiralty in 1888. In this Manual conditional contraband embraces provisions and liquors fit for consumption of army or navy; money; telegraphic materials, such as wire, porous cups, platina, sulphuric acid, and zinc ; materials for railway construction, as iron bars and sleepers; coals, hay, horses, rosin, tallow, and tim- ber. But these articles, it is stated, " are contraband only in case it may be presumed that they are intended to be used for the pur- poses of war," and " this presumption arises when such hostile destination of the vessel is either the enemy's fleet at sea, or a hos- tile port used exclusively or mainly for naval or military equipment." On the outbreak of the war with Japan, the Russian government, in March, 1904, published instructions to its naval commanders which forbade the conveyance of contraband " to Japan or to Japa- nese armed forces," and denounced as contraband " foodstuffs," including all kinds of grain, fish, fish products of various kinds, beans, bean oil, and oil cakes. The British government protesting expressed " great concern " that " rice and provisions " should be treated as unconditionally contraband, this being regarded " as in- consistent with the law and practice of nations." The British gov- ernment, it was declared, did not contest " that, in particular cir- cumstances, provisions may acquire a contraband character, as for instance, if they should be consigned direct to the army or fleet of a belligerent, or to a port where such fleet may be lying " ; but it 36 MOORE— CONTRABAND OF WAR. [February 2, could not admit " that if such provisions were consigned to the port of a belligerent (even though it should be a port of naval equip- ment) they should therefore be necessarily regarded as contraband of war." The true test appeared to be " whether there are circum- stances relating to any particular cargo to show it that it is destined for military or naval use." The United States was obliged to deal with the same question in the case of the steamer Arabia, whose cargo, composed of rail- way material and flour, destined to Japanese ports and consigned to various commercial houses there, was condemned by the Russian prize court at Vladivostok as contraband, on the strength of its destination. The United States protested against this judgment as involving a " disregard of the settled law of nations." The United States declared that it was " vital to the legitimate maritime com- merce of neutral states" that there should be "no relaxation" of the distinctions with regard to contraband ; that there was and could be " no middle ground " ; that " the criterion of warlike usefulness and destination " had " been adopted by the common consent of civi- lized nations, after centuries of struggle in which each belligerent made indiscriminate warfare upon all commerce of all neutral states with the people of the other belligerent, and which led to reprisals as the mildest available remedy " ; that, while articles such as arms and ammunition, self-evidently of war-like use, were contraband if destined to enemy territory, yet articles such as coal, cotton, and provisions, which, though ordinarily innocent, were capable of war- like use, were " not subject to capture and confiscation unless shown by evidence to be actually destined for the military or naval forces of a belligerent " ; that " this substantive principle of the law of nations" could "not be overridden by a technical rule of the prize court that the owners of the captured cargo must prove that no part of it" might reach the enemy forces; and that, such proof being "of an impossible nature," its exaction would render neutral commerce impossible and result in the condemnation of the innocent with the guilty. In conclusion the ambassador of the United States at St. Petersburg was instructed to express "the deep regret and grave concern " with which his government had received the unqualified '912.] MOORE— CONTRABAND OF WAR. 37 communication of the decision of the prize court, and was directed to " make earnest protest against it " and to say that his government regretted " its complete inabihty to recognize the principle of that decision and still less to acquiesce in it as a policy." In consequence of the British and American protests the Russian government appointed a commission to consider the question of con- traband, and on October 22, 1904, announced that, while horses and beasts of burden would continue to be treated as contraband of war, yet various other articles, including rice and foodstuffs, would be considered as contraband if destined for a belligerent government, its administration, army, navy, fortresses, naval ports, or purveyors, but not if " addressed to private individuals." Since the war between Russia and Japan, the subject of contra- band has been dealt with in the Declaration of London, signed Feb- ruary 26, 1909, by representatives of Germany, the United States, Austria-Hungary, Spain, France, Great Britain, Italy, Japan, the Netherlands, and Russia, with the object of laying down rules of maritime law, embracing blockade, contraband, unneutral service, destruction of neutral prizes, and various other subjects, for the government of the International Prize Court which Germany pro- posed to the Second Peace Conference at The Hague, and for the constitution of which provision was made by the convention signed on October 18, 1907. As the House of Lords has lately rejected a bill, which had passed the Commons, to carry this convention into effect, the fate of the Declaration must, so far as Great Britain is concerned, be regarded as at least doubtful. It has been fiercely assailed in England, but has been ably defended by eminent persons, among whom Westlakemay be particularly mentioned, who, although they naturally do not pronounce it perfect, consider that its adop- tion would on the whole be advantageous. Into this general ques- tion it is beyond jny province now to enter, my subject being simply contraband. The Declaration (Article 24), following the Grotian classifica- tion, divides articles into (i) absolutely contraband, (2) condition- ally contraband, and (3) absolutely noncontraband. The second category — the conditionally contraband — includes fourteen general 38 MOORE— CONTRABAND OF WAR. [February 2. heads, namely, foodstuffs ; forage and grain, suitable for feeding animals ; clothing, fabrics for clothing, anrl boots and shoes, suitable for use in war; gold and silver in coin or bullion, and paper money; vehicles of all kinds available for use in war, and their component parts; vessels, craft, and boats of all kinds,-^ floating docks, parts of docks and their component parts ; railway material, both fixed and rolling-stock, and materials for telegraphs, wireless telegraphs, and telephones ; balloons and flying machines and their distinctive component parts, together with accessories and articles recognizable as intended for use in connection with balloons and flying machines ; fuel, and lubricants ; powder and explosives not specially prepared for use in war ; barbed wire and implements for fixing and cutting it ; horseshoes and shoeing materials ; harness and saddlery ; field glasses, telescopes, chronometers, and all kinds of nautical instru- ments. And to this list belligerents are (Article 25) allowed to add by declarations notified to other powers. For all contraband the Declaration preserves (Article 39) the penalty of condemnation; and it provides (Article 33) that "condi- tional contraband" shall be liable to capture if "destined for the use of the armed forces or of a government department of the enemy state, unless in this latter case the circumstances show that the articles cannot in fact be used for the purposes of the war in progress." As to proof of destination, the provisions of the Decla- ration are two-fold. The doctrine of continuous voyage, though declared to be applicable to absolute contraband, is not applied to conditional, so that cargoes of the latter are not put in jeopardy when sent to a neutral port. This is a desirable and important safe- guard. A hostile destination is, on the other hand, presumed (Arti- cle 34) " if the consignment is addressed to enemy authorities, or to a merchant, established in the enemy country, and when it is well ^ This provision that vessels, craft and boats shown to be intended for belligerent use may be seized and confiscated as contraband evidently is not intended to alter or modify the lavi^ according to which the fitting out, arming, or equipping in neutral jurisdiction of a vessel to cruise or carry on war against one of the belligerents constitutes, not a mere transaction in contra- band, but the setting on foot of a hostile expedition, which the neutral is bound to use due diligence to prevent. 1912] MOORE— CONTRABAND OF WAR. 39 known that this merchant suppUes articles and material of this kind to the enemy," or " is destined to a fortified place of the enemy, or to another place serving as a base for the armed forces of the enemy." These grounds of inference are so vague and general that they would seem to justify in almost any case the presumption that the cargo, if bound to an enemy port, was " destined for the use of the armed forces or of a government department of the enemy state." Any merchant established in the enemy country, who deals in the things described, will sell them to the government; and if it becomes public that he does so, it will be " well known " that he supplies them. Again, practically every important port is a " forti- fied place " ; and yet the existence of fortifications would usually bear no relation whatever to the eventual use of provisions and various other articles mentioned. Nor can it be denied that, in this age of railways, almost any place may serve as a " base " for sup- plying the armed forces of the enemy. And of what interest or advantage is it to a belligerent to prevent the enemy from obtaining supplies from a " base," from a " fortified place," or from a mer- chant " well known " to deal with him, in his own country, if he is permitted freely to obtain them from other places and persons, and especially, as countries having land boundaries can for the most part easily do, through a neutral port? No doubt the advantage of such prevention may readily become greater, if the enemy be, like Great Britain or Japan, an insular country. The attempt to establish an international prize court constitutes one of the most remarkable advances ever proposed towards the founding of an international jurisdiction, and the efifort made in the Declaration of London to furnish a universal law is a step in the right direction. The able framers of the Declaration may be assumed to have made the best compromise that was at the time obtainable. But the question of contraband remains unsolved; and it will so remain either until, by an inconceivable relapse into primi- tive sixteenth-century conditions, all commerce with belligerents is forbidden, or until innocent articles of universal use, such as pro- visions, which, even when consumed by military men, are consumed by them as human beings rather than as soldiers, are, in conformity 40 MOORE— CONTRABAND OF WAR. [Februarys, with the traditional contention of the United States, put beyond reach of capture on loose and interested surmises. While seizures of articles commonly classed as conditional con- traband have inflicted upon neutrals enormous losses, the effect of such seizures upon the fortunes of the belligerents has by no means been so appreciable as it is often hastily assumed to have been. Lawless, unrestrained and successful as were the depredations on neutral commerce during the wars following the French Revolution, not only did the struggle persist through more than twenty years, but its end was scarcely hastened by the spoliations, which indeed seem rather to have supplied the means of its prolongation. The reduction of the South, during the American Civil War, was sen- sibly accelerated by the cutting off of its commerce, but this result was achieved chiefly by means of blockade. At the Second Peace Conference at The Hague, in 1907, the British government, with a view to diminish the difficulties which neutral commerce encounters in case of war, proposed that the powers should enter into an agreement to abandon the principle of contraband altogether, and to confine the right of visit to the ascer- tainment of the merchant vessel's neutral character. Such a meas- ure was justified on the ground that, while it had in spite of all efforts been found to be impossible to prevent belligerents from obtaining the munitions which they needed, the attempt to do so had, by reason of the increase in the tonnage of ships, the carrying of mixed cargoes, the lack of any single destination of ship or cargo, the multiplication of the number of articles used in war, and the development of railways and other means of transportation by land, become more and more futile on the part of belligerents and more and more injurious to neutrals. The circumstance that the radical proposal of Great Britain, although it was not eventually adopted by the Conference, received the support of twenty-six of the powers represented therein, while only five voted against it,-^ alone suffices ^For: Argentine Republic, Austria-Hungary, Belgium, Brazil, Bulgaria, Chile, China, Cuba, Denmark, Dominican Republic, Great Britain, Greece, Italy, Mexico, Netherlands, Norway, Paraguay, Peru, Persia, Portugj^l, Salva- dor, Servia, Siam, Spain, Sweden, Switzerland. — 26. Against: France, Germany, Montenegro, Russia, United States. — 5. 19 12.] MOORE— CONTRABAND OF WAR. 41 to demonstrate the existence of a general conviction that the present state of things is altogether unsatisfactory. Recalling the treaties between Prussia and the United States of 1785 and 1799 for the virtual abolition of contraband, it is curious to find the United States and Germany acting together as two of the five powers that voted against its abolition in 1907; but, although the United States voted against the British proposal, it is gratifying to note that Admiral Sperry, on behalf of the United States delegation, after the British proposal had failed to secure the unanimous ap- proval of the conference, maintained the historic American position that the right of capture should be confined to articles agreed to be absolutely contraband. In this relation it may be observed that the Institute of International Law, in 1896, after much deliberation, voted that the category of conditional contraband should be abolished, the belligerent, however, to have the right, at his pleasure and subject to an equitable indemnity, to sequester or to preempt, when on their way to an enemy port, articles serving equally for war and for peace."" Rather than allow existing conditions to continue, it might be advisa- ble to add to the present duties of neutrals the obligation to prohibit the exportation of aid Mineralogie, Vol. 28, pp. 1-35, 414- 451 (1857). Abstract by Moses, School of Mines Quarterly, Vol. 25, pp. 415-420 (1904). ^* Hermann, Zeitschrift fiir Mineralogie, Vol. 39, p. 478 (1904). 114 ROGERS— THE VALIDITY OF [March i, than the b-a.xis. Out of 59 monoclinic minerals with a less than unity, (010) occurs on 56, but (100) on only 46 while (120) occurs on 23, but (210) on only 13. Out of 64 monoclinic minerals with a greater than unity, (100) occurs on 60, but (010) on only 43 while (210) occurs on 16, but (120) on only 13. If a is shorter than b, the molecules are more closely packed along (010) and (120) than along (100) and (210), but if a is longer than b the reverse is true. Out of 168 combinations of orthoclase (including microcline) crystals given in Hintze's " Handbuch der Mineralogie," (010) 100 Fig. 4. The probable structure of orthoclase. occurs on 133, but (100) on only 22. The form (130) occurs 70 times but (120) occurs only once! This remarkable case is ex- plained by assuming the structure to be that of the monoclinic or clinorhombic prism, one of the space-lattices of Bravais. It can be seen from Fig. 4 that the molecules are more closely spaced along (130) than along (120). It is certainly true that the form-series differs for various crys- tals, but according to the law of complication the form-series should be alike for all crystals and all systems. ^^ For those who are familiar with chemistry, the whole matter of indices, rationality, crystal structure, and relative frequency of crystal faces may be cleared up by considering the analogy between the fundamental laws and theories of chemistry and those of crys- tallography. " Goldschmidt (Joe. cif.) explains the differences in the form-series by assuming outer disturbing influences. These undoubtedly have an effect but certain discrepancies are more easily explained by the law of maximum reticulate density. 1912.] THE LAW OF RATIONAL INDICES. 115 For the crystals of any one substance the angles between corre- sponding faces are constant. This law is known as the law of constancy of interfacial angles. It corresponds to the law of defi- nite proportions in chemistry. The proportions in which two elements combine determines the atomic weight of the elements. In an analogous way the intercepts, which are determined by certain constant interfacial angles, establish the axial ratio which, like the atomic weight, is a constant. Crystal measurement corresponds to quantitative analysis in chemistry. Exact measurements establish the axial ratio of a crys- tal just as exact analyses establish the atomic weight of an element. Two chemical elements A and B unite not only to form the com- pound AB but also the compounds ABr,, A.Mz> A^B, etc. This fact is known as the law of multiple proportions. These proportions for most chemical compounds are usually simple but in many com- pounds, especially those containing silicon or carbon, they are often far from simple. Among silicate minerals we have such compounds as MggAljjSi^OoT and H^oMg^^^AlgSieO^^. Among organic com- pounds we have C6oHi22> C17H23NO3, Co^¥{^QO^^, and many others with fifty or more carbon atoms in the molecule. In spite of these complex formulje all chemists accept the law of multiple propor- tions as an established fact. Without it chemistry would scarcely deserve to be called a science. The law of rational indices in crystallography corresponds to the law of multiple proportions in chemistry. The same difificulties are encountered in crystal meas- urement as in quantitative analysis. That is, there are certain errors which usually render it impossible to prove absolutely the law of rational indices or the law of multiple proportions.-*' According to Jaquet the formula of hemoglobin (of the dog) is C-5SH1003N195- S3FeOois- This formula can hardly be regarded as established. It may be a little different but it is very probable that these elements unite in definite proportions. This is exactly analogous to vicinal faces such as (251 •250-250) observed on alum by Miers. The law of multiple proportions was deduced by Dalton from his atomic theory before there were accurate analyses to prove it, ■" Organic chemistry has an advantage over inorganic chemistry in that the formulse may usually be determined by the method of formation. 116 ROGERS— THE VALIDITY OF [March i, just as the law of rational indices was deduced by Haiiy from his theory of crystal structure. If chemical compounds are made up of atoms they must necessarily unite in definite proportions. This it will be recalled is precisely analogous to the argument used for proof of the rationality of the indices. If crystals are made up of particles or molecules, the crystal faces necessarily have rational indices. Two or more given elements do not unite in all possible pro- portions but in a comparatively few, usually simple, proportions which we explain by the term valence. There are but two oxids of mercury Hg.O, and HgO which we explain by saying that the valence of mercury is one and two. This is analogous to the limita- tion imposed by the law of complication of Goldschmidt or the law of maximum reticulate density of Bravais. To complete the analogy between the laws and theories of crys- tallography and chemistry let us consider the periodic law and its analogue. Alendeleef, the Russian chemist, predicted the existence of several chemical elements, scandium and gallium, which he called ekaboron and eka-aluminum, before they were discovered. Not less remarkable was the deduction by Hessel, a German mathematician, ^ of the thirty-two possible types of symmetry in crystals, assum- ing 2-, 3-, 4-, and 6-fold symmetry-axes, in 1830, at a time when only about half of them were known. Of the thirty-two possible types of symmetry, only one remains to be found. Summary. Judging from various text-books and articles a difference of opinion exists as to the exact meaning of the law of rational indices. Some authors limit the indices to simple numbers while others admit that occasionally the indices are large numbers. Unfortu- nately this question can not be decided by direct measurement of the angles on account of errors in measurement. As crystals possess axes of only 2-, 3-, 4-, and 6-fold symmetry they must consist of regularly arranged molecules, or particles of some sort, whatever their nature may be. Crystal faces, then, necessarily have rational indices. The indices are usually small numbers but may also be '912.] THE LAW OF RATIONAL INDICES. 117 complex, the complexity in general increasing with the rarity of the face. The structure theory of Bravais offers a satisfactory ex- planation of the abundance of faces with simple indices and the rarity of faces with complex indices. There is a remarkable analogy between the fundamental laws of chemistry and crystallography. Stanford University, California, Feb., 1912. PROC. AMER. PHIL. SOC, LI. 204 E, PRINTED JUNE 5, I9I2. DYNAMICAL THEORY OF THE GLOBULAR CLUSTERS AND OF THE CLUSTERING POWER INFERRED BY HERSCHEL FROM THE OBSERVED FIGURES OF SIDEREAL SYSTEMS OF HIGH ORDER. By T. J. J. SEE. (Read April /p, 1012.) (Plates VIII (bis) and IX.) I. Introductory Remarks. More than a century and a quarter have elapsed since it was con- fidently announced by Sir William Herschel that sidereal systems made up of thousands of stars exhibit the effects of a clustering power which is everywhere moulding these systems into sym- metrical figures, as if by the continued action of central forces (Phil. Trans., 1785, p. 255, and 1789, pp. 218-226). In support of this view he cited especially the figures of the planetary nebulae, and the globular clusters, as well as the more expanded and irregular swarms and clouds of stars visible to the naked eye along the course of the Alilky Way, which thus appears to traverse the heavens as a clustering stream. And yet notwithstanding the early date of this announcement and the unrivaled eminence of Herschel, it is only very recently that astronomers have begun to consider the origin of sidereal systems of the highest order. The historical difficulty of solving the problem of n-bodies, when n exceeds 2, which dates from the establishment of the law of universal gravitation by Newton in 1687, will sufficiently account for the restriction of the researches of mathematicians to the plane- tary system, where the central masses always are very predominant, the orbits almost circular and nearly in a common plane, and to other simple systems such as the double and multiple stars : but owing to the general prevalence of the clustering tendency pointed out by Herschel and now found to be at work throughout the sidereal uni- 118 1912.] OF THE GLOBULAR CLUSTERS. 119 verse, it becomes necessary for the modern investigator to consider also the higher orders of sidereal systems, including those made up of thousands and even millions of stars. It is only by such a com- prehensive view of nature, which embraces and unites all types of systems under one common principle, that we may hope to establish the most general laws governing the evolution of the sidereal universe. Accordingly, although the strict mathematical treatment of the great historical problem of 7J-bodies is but little advanced by the recent researches of geometers, yet if we could arrive at the general secular tendency in nature, from the observational study of the phe- nomena presented by highly complex systems of stars, operating under known laws of attractive and repulsive, forces, the former for gathering the matter into large masses, the latter for redistribut- ing it in the form of fine dust, the result of such an investigation would guide us towards a grasp of problems too complex for rigor- ous treatment by any known method of analysis. Now it happens that in the second volume of the " Researches on the Evolution of the Stellar System," 1910, the writer was able to establish great generality in the processes of cosmogony, and to show that the universal tendency in nature is for the large bodies to drift towards the most powerful centers of attraction, while the only throwing off of masses that ever takes place is that of small particles expelled from the stars under the action of repulsive forces and driven away for the formation of new nebulae. The repulsive forces thus operate to counteract the clustering tendency noticed by the elder Herschel, and so clearly foreseen by Newton as an inevitable effect of universal gravitation upon the motions of the solar system that he believed the intervention of the Deity eventually would become necessary for the restoration of the order of the world (cf. Newton's "Letters to Bentley," Brewster's "Life of Xewton," Vol. IL, and Chapter XVIL, and Appendix X). But wdiilst the argument developed in the second volume of my "Researches" gives unexpected simplicity, uniformity and continuity to the processes of cosmogony, there has not yet been developed, so far as I know, any precise investigation of the attractive forces oper- ating in globular clusters, which might disclose the nature nf the 120 SEE— DYNAMICAL THEORY [Ap^ii '9, clustering power noticed by Herschel to be in progress throughout the sidereal universe. Such an investigation of the central forces governing the motions in clusters is very desirable, because it might be expected to throw light on the mode of evolution of clusters as the highest type of the perfect sidereal system. If it can be shown that a clustering power is really at work, and is of such a nature as to produce these globular masses of stars, it will be less important to consider the details of those systems which have not yet reached a state of symmetry and full maturity ; for the governing principle being established for the most perfect types, it must be held to be the same in all. II. General Expressions for the Potential of an Attracting Mass. If we have a mass M' of any figure whatever, in which the law of density is a' = f{x' ,y' ,z'), where (.r',3'',^') are the coordinates of the element dm' of the attracting mass, and this element attracts a unit mass whose coordinates are {x,y,z) ; then the element of the attractmg mass is dm' = for the longitude, 6 for the latitude, and r for the radius of the sphere ; and then the required expressions become x' — X == r sin 6 cos ^, y' — 3' ^ r sin ^ sin . ( 5 ) The element of the potential due to this differential element is o-';'^ sin ddrddd^ r and the general expression for the potential becomes (6) U=^ r\i4> r smdde r a'rdr. (7) 4^^ Jo Jo Jo If we make use of the equations (i), (4), (5) in equation (2) we may obtain the corresponding expressions for the forces resolved along the coordinate axes : X= f\os f sm-ddd f a'dr, Jo t/o i/o F= r " sin (^d<^ r sin^ Odd f a'dr, (8) ♦/O t/O I/O Z= f^dcf) r cos d sin dde f a'dr. t/O t/o t/0 These expressions will hold rigorously true for any law of density whatever, so long as it is finite and continuous. In the physical universe these conditions always are fulfilled ; and hence if these sev- eral integrals can be evaluated, they will give the potentials and forces exerted on a unit mass by an attracting body such as a cluster of stars, or the spherical shell surrounding the nucleus of a cluster. But before considering the attraction of a cluster in detail, we 122 SEE— DYNAMICAL THEORY [April 19, shall first examine the cumulative effect of central forces on the law of density. The problem is intricate and must be treated by methods of great generality, but as it will elucidate the subsequent procedure for determining the attraction of such a mass upon a neighboring point, we shall give the analysis with enough detail to establish clearly the secular effect of close appulses of individual stars upon the figure and internal arrangement of these wonderful masses of stars. III. The Cumulative Effect of the Central Forces upon the Figure and Compression of a Globular Cluster of Stars. Suppose a globular cluster of stars to be in a moderate state of compression, with density increasing towards the center. Imagine the whole of the mass at the epoch ^^ to be divided into two parts by a spherical surface of radius r, drawn about the center of gravity of the entire system ; and let the external boundary of the cluster be R, so chosen that no star, from the motions existing at the initial epoch, will cross the border r = R. The stars in the outer shell, between the surfaces r and R, with coordinates (-v', 3'',-'), will give rise to a potential U . Those of the nucleus or series of internal shells, be- tween r = o, and r^=r, with coordinates {x,y,z), will give rise to a potential V. Accordingly we have , , , a'dx'dy'dz' Vix' - xy -^ {y -yf + {z' - zY = /// , C C C (Tdxdydz J J J Vix' — X (9) V{x' - xf ^ {/ - yf + {z' - zf And the forces resolved along the coordinate axes are ^^ Y C C C (T'{x'—x)dx'dydz' ^ ^ " ~ J J J \\x' - xf + [y' - yf +\z' - zf ^7" J J J [(;r'-;r)^ + (y-jf + (y-.^fji' ^'°) •^^ -y CCC ^ x'" x'' x'" x' Vx'^ x'" x^ ^ "I LT~2o "^240 "3888"^ "J ,.4 ,.6 (38) _ ''" 1 3 ~ 20 + 240 ~ 3^888 + • • • f ~ \\ x'" x'' x'' 1 ■ ■'' |3~20 + 24o"~3S88+*""J As the coefficients of the series jx and fx are the same, we may cal- culate from the equation (37) or (38) the value of the ratio at suitable intervals throughout the sphere, and ascertain rigorously the law of the variation. The results of my calculations are given in the following table and illustrated by the corresponding curve in Fig. I. 136 SEE— DYNAMICAL THEORY [April 19, Table Showing Decrease of Centr.\l Gravity in a Sphere of Monatomic Gas in Convective Equilibrium. The Decrease of Central Gravity in a Globular Cluster is Slightly Less Rapid, Owing to Greater Accumulation of Density Towards the Center. ijstance from Center. Ratio of Internal Gravity to Surface Gravity. " x' _ C ~ G I.O 1. 00000 0.9 0.92563 0.8 0.84378 0.7 0.75495 0.6 0.65975 0.5 0.55928 0.4 0.45317 0.3 0.34769 0.2 0.23069 0.1 0.1 1587 0.0 0.00000 VI. Dynamical State of a Globular Cluster. In works on the theory of potential and attraction the following theorems are demonstrated and well known : 1. That a sphere either homogeneous or made up of concentric spherical shells attracts an external point as if collected at its center (Newton's " Principia," Lib. I., Prop. LXXVL, Theorem XXXVI. ). 2. That homogeneous spherical shells attract external points as if collected at their centers of figure, and exert no attraction on points within ("Principia," Lib. I., Prop. LXX., Theorem XXX.). Also a point within the sphere is attracted by a force proportional to the distance from the center (" Principia," Lib. I., Prop. LXXIIL, Theorem XXXIII.) ; and the same theorem holds for the spheroid made up of concentric spheroidal shells ("Principia," Lib. I., Prop. XCL, Prob. XLV.). 3. That ellipsoidal hoiiia-oids, or ellipsoidal shells of any thick- ness made up of homogeneous layers, bounded by two ellipsoidal surfaces, concentric, similar and similarly placed, likewise exert no attraction on points within, as is shown by Newton in the " Prin- cipia " (Lib. I., Prop. XCL, Prob. XLV., Cor. 3) for the case of the spheroid, which corresponds to the figure and internal arrange- ment of density in such bodies as the planets, sun, and stars. '912.] OF THE GLOBULAR CLUSTERS. 137 To illustrate the simple case of a homogeneous sphere^ we re- mark that it attracts a point at its surface with a force /= ^-j,2 =^'^<^''=Cr, (39) where o- is the density, and r the radius. This equation shows that all points within the sphere are attracted to the center by forces proportional to the radii of the shells on which they are situated, since the external shells exert no attraction on points within. Let the solid sphere be set rotating steadily about an axis ; then as the central forces at the various points are proportional to the radii described by the points, there will be no tendency arising from the central attraction for any shell to be displaced with respect to the shells within or without, once the condition of equilib- rium is attained, but the central accelerations will everywhere tend to secure steady motion without relative displacement of the parts of the sphere. The same is true of the centrifugal force, after the adjustment to a suitable figure of equilibrium; for the centrifugal force is equal to v'/r, v being the velocity of the particle and r the radius it describes ; for this gives v"^ {T.irrf \TTr and as it is common for all particles the force has the same form here as in equation (39). What is here proved for the simple case of the homogeneous sphere, will obviously hold also for a sphere made up of concentric spherical shells of uniform density; for the theorem will hold for all the points within. And similarly for ellipsoidal honiaroids, or sphe- roids such as the planets, sun and stars. If any of these masses have attained uniform movement as of rotation, there is no tend- ency to produce a relative displacement of the parts. Now the simple equation (39) shows that a similar theorem holds for the internal dynamics of a globular cluster, the component stars of which have attained a state of equilibrium following a definite law of density depending only on the radius. But before 138 SEE— DYNAMICAL THEORY [April 19, treating of this at length, we shall recall a suggestive investigation of Sir William Herschel printed in the Philosophical Transactions for 1802 (pp. 477-502) under the title " Catalogue of 500 New Nebulze, Nebulous Stars, Planetary Nebulse, and Clusters of Stars; with Re- marks on the Construction of the Heavens." VII. Herschel's Theorem on the Motion of Multiple Stars, 1802. In the important paper just cited Herschel first discusses " Binary Sidereal Systems or Double Stars," and then proceeds to Section " III. Of more complicated sidereal systems, or treble, cjuad- ruple, quintuple and multiple stars," where he reasons as follows : " In all cases where stars are supposed to move round an empty center, in equal periodical time, it may be proved that an imaginary attractive force may be supposed to be lodged in that center, which increases in a direct ratio of the distances. For since, in different circles, by the law of centripetal forces, the squares of the periodical times are as the radii divided by the central attractive forces, it follows, that when these periodical times are equal, the forces will be as the radii. Hence we conclude, that in any system of bodies, where the attractive forces of all the rest upon any one of them, when reduced to a direction as coming from the empty center, can be shown to be in a direct ratio of the distance of that body from the center, the system may revolve together without perturbation, and remain permanently connected without a central body." This reasoning is best understood by means of simple formulae: Let /i and /o be two centrifugal forces, which in revolving systems are always equal to the centripetal forces, and F^ and Vo the cor- responding velocities of the bodies, and i\ and To the radii of the circles in which they are supposed to revolve. Then, by the ele- mentary principles of mechanics, we have fi= ,. ; A = -- ; whence/, == -yj— ; /, = -.,— - . 1 2 11 22 This gives /2 4'^'^'i. .2_4tV2 .^,N A =— ^, ^2 =-y-— • (41) Now in orbital revolution the centripetal and centrifugal motions 1912.] OF THE GLOBULAR CLUSTERS. 139 are always exactly equal, and hence if tj^^t.,, we have whence ^2 ^2 ^2 ^1 — or — A-rr' A ' A A A r, A-rr,' (42) as concluded by Herschel in the Philosophical Transactions, for i8o2, p. 487. To establish clearly such actual cases of motion, with the attract- ive force in the direct ratio of the distance from the empty center, where he says the system may revolve together without perturba- tion, and remain permanently convected without a central body, Herschel proceeds to deal first wath two equal double stars re- volving in circles about the common center of gravity of the sys- tem. He next generalizes the procedure by taking two unequal masses, then treats also the cases of motion in elliptic orbits, and finally considers certain types of triple and multiple stars, to which similar reasoning will apply. This paper of Herschel is quite re- markable, and deserving of more attention than it has received. VHI. Theorem on the Revolutions of Stars in Clusters. It is now obvious that the clusters which have attained a definite law of density depending wholly on the radius will conform to Herschel's Theorem of motion about empty centers, which is also the law for the central motion of particles of a rotating solid. H we imagine a heterogeneous sphere made up of concentric homo- geneous layers, but with the density of the layers increasing towards the center, and take the radii of the layers to be r-^, r^, r^, . . . Vi, and denote by o-^, a^, 0-3, .. . ai the average density of the sphere up to the ith layer inclusive ; then the attraction on points in these several layers will be A^, A^, A^, . . . Ai, as follows: 4 TTO" T ^ A = - -^2- = ^1^ ; ^2 = Q\ ; A = Q\ ; • • • ; ^.■= Q;- (43) 3 ' 1 Thus the constant will vary from layer to layer in a heterogeneous 140 SEE— DYNAMICAL THEORY [April 19, sphere made up of concentric homogeneous shells, but the attraction at every point, including the external surface, is proportional to the radius of the shell in cjuestion. Now just as a sphere, either homogeneous or made up of con- centric layers of uniform density, attracts all internal points, in- cluding those at the external surface, with a force proportional to the radius of the shell on which it is situated; so also will a cluster which is condensed towards the center according to any law of density depending wholly on the radius, attract all internal points, including those in the external surface, according to the same law of direct proportionality to the distance from the center. When the attractive force varies directly as the distance from the center, the particle so attracted describes an ellipse as was first proved by Newton in the " Principia " (Lib. I., Prop. X., Prob. V.). This case of attraction depending directly on the first power of the distance is also discussed by the analytical method in Vol. II. of my "Researches," 1910, pp. 25-27, where it is shown that the time of revolution is quite independent of the dimensions of the ellipse, but depends wholly on the intensity of the central force. For motion in a plane the coordinates of the particle are shown to be defined by the equations : V cos -Jr . — — V sin -ylr — X — = — sm y lit -\- a cos V ixt, y = ^— sm v [it. (44) V ii v> As the values of the coordinates are the same at the time t and 27r _ ^ . . . 27r ^ -f- — ~- it is evident that the time of revolution is — — , or inversely V/^' VM as the square root of /x, where /x is the mass, and exerts the corre- sponding unit of force at unit distance. In a cluster with stars arranged according to a law of density depending wholly on the radius, the value of \i. or the force will depend wholly on the radius also, as shown in equation (34). And thus the time of revolution will be independent of the dimensions of the ellipse. Assuming that there is but little relative displacement of the bodies of the clusters, a star situated, therefore, in an outer I9I2.] OF THE GLOBULAR CLUSTERS. 141 shell will revolve about the common center of gravity in exactly the same time as one situated near the center ; for the remoter stars revolve under a greater attractive force, while the nearer ones revolve under feebler forces, and all would therefore have a com- mon period. The movement at the end of the period would restore the cluster to its original state, the individual bodies being exactly where they started from at the initial epoch. This is one of the most remarkable results of the dynamics of a system of n-bodies arranged in concentric shells of uniform density, depending wholly on the radius, as in our typical globular clusters, which are made up of stars of equal brightness and apparently of equal mass. If therefore the cluster were once established with such rela- tions among the stars that their orbits do not intersect, and the sphere of powerful attraction for each star is small compared to the spaces between the neighboring stars, the wonderful system thus arranged might oscillate in stability for millions of ages. These conditions evidently are quite fully realized in the globular clusters, as will more clearly appear from the following considerations on their mode of formation. IX. The Symmetrical Growth of a Cluster due to a Process OF Internal Compensation. In the second volume of my " Researches," 1910, it is shown by a line of argument based on the principle of continuity, similar to that used by Herschel in the Phil. Trans., 181 1, p. 284, that the nebulae are formed by the gathering together of dust expelled from the stars under the action of repulsive forces. As this dust gathers towards a center so as to form a nebula or cluster, of more or less symmetrical figure, it takes a long time for the new system to acquire an arrangement by which the density increases from the surface to the center. In the course of ages, however, the central mass in- creases or the central group of masses accumulate, by accretion of dust to the individual bodies, or by the capture and redistribution of interpenetrating bodies. The result, on the one hand, is that all orbits will be decreased in size and the system will contract its di- mensions ; and, on the other hand, this waste matter will tend to ac- 142 SEE— DYNAMICAL THEORY [April 19, cumulate in regions of stability, and there build up the smaller into larger bodies. Thus the individual stars being supplied from such varied sources the cluster will necessarily acquire increasing sym- metry, and orderly arrangement, like those actually observed. This natural tendency to order and stability will be greatly aug- mented by mutual compensation among the stars of the cluster. As the stars are both gaining and losing matter incessantly, under the mutual interaction of attractive and repulsive forces, it is evident that those which gain too rapidly, will also begin at once to lose at an abnormal rate, owing to the augmented action of the repulsive forces ; and the dust expelled from them will go directly or indirectly very largely to the other members of the cluster, and thus operate to restore the equilibrium of the whole group. Moreover, if any serious collision occurs, by which one star acquires predominant size, it will at the same time acquire such abnormal energy of radiation, that the balance of power will tend to become gradually restored under the action of the repulsive forces at work. From these known causes one would expect a cluster therefore to be a mutually compensating system, producing and building up new bodies in vacant regions, where the conditions are stable, and redistributing undue accumulations of mass by the natural balance established between attractive and repulsive forces, as all the stars gain matter from surrounding space and again expel it after a cer- tain repulsive vigor has been attained. The eventual accumulation of so many stars in a comparatively small space largely operates to retain the dust expelled from them in that region; it thus goes to other members of the group, rather than to the rest of the remote stars of the universe, so that in the course of vast time — millions of ages in Herschel's expressive phrase — the cluster accumulates to such grandeur and order as we see in such noble globular clusters as that in Hercules, 47 Toucani, and Omega Centauri. It is worthy of note that this simple theory, based on known and established laws, explains not only the origin and growth of these wonderful masses of stars, under conditions of stability ; but also the nearly perfect equality of the individual stars which has always been so bewildering to astronomers. 1912.] OF THE GLOBULAR CLUSTERS. 143 X. How A Star Entering a Cluster has its Oscillations Damped and is Finally Captured. If we recall the familiar equations for an oscillation, as treated in works on physics, r) = ae~''^ cos (lit -\- a), or ■,j=zae'''^ sm(nt-\-p), (45) where a is the original amplitude of the harmonic oscillation, so that a^"'' ' becomes a coefficient decreasing as t increases, 11 =^ 2Tr/T, T being the period ; we see that as the time f increases the ordinate rj will decrease, though the period T remains constant. The equation (45) thus represents a damped vibration, such as constantly arises where resistance is encountered by vibratory motion. Under these circumstances the harmonic curve rapidly loses amplitude and is of the form : Fig. 2. Illustrating damped vibrations. The process of damping here brought to light for oscillating particles describing simple harmonic motion has its analogies in the movements of stars in a cluster ; for here too the period of the movement, as we have seen in VIII., is essentially constant, but the amplitude of the oscillation is reduced till it becomes adapted to that of the rest of the system. This is a part of the capture process, because it tends to reduce all the abnormal movements to one dead level. Let us now examine the dynamical process by which stars tend to become entrapped in the central region of a cluster. If we con- sider the potential of a spherical shell of stars obeying any law of 144 SEE— DYNAMICAL THEORY [April 19, density, and having a thickness R-r, it is evident from equation (7) that V =^ r "" d4> r sin ddd f ardr, (46) and the forces along the coordinate axes will be X' = f cos (f)d(f) r sin^ OcW f adr, y = f sin r sin' Ode f adr, (47) Jo Jo Jr Z' ^ { dcf) f cos e sin OdO f adr. Now every globular cluster may be regarded as made up of a series of such shells; so that the total forces become X=Yi A". = Z cos c\>dci) sin- Odd adr, i = \ 1 = 1 Jo Jo Jr y=T,^i = 12 r " sin (^# psin' Ode f adr, (48) »=1 ! = 1 Jo Jo J I- Z=Y. = Z d(l) \ cos e sin ede adr. i=.\ i = l t/o t/o Jr These expressions are so complex, that we are obliged to re- strict our consideration to the action of a single shell. Accordingly, we shall suppose the single shell filled with stars to a considerable density, and the distribution uniform. An external star coming in from the distance, if otherwise undisturbed, will revolve in a Kep- lerian ellipse having its focifs in the center of the shell. The mass acting as if collected at the center is 4710-;'- (i?-r), where the thickness R-r is not too large ; and the velocity accjuired at the outer border of the shell is V^^k^i^-rrarXR-r)]^--'^, (49) where a is the semi-axis major of the Keplerian ellipse. I9I2.] OF THE GLOBULAR CLUSTERS. 145 As soon as a part of the shell of thickness dr has been traversed, however, the stars included in the space ^irr-dr will cease to exert at- traction on the moving star; and the further it enters the shell the less central attraction will be exerted from the original focus. As the star quits the shell and enters the hollow space within there will be no central attraction to cause it to describe a Keplerian ellipse. Thus as the radius vector decreases from R to r, the path ceases to be the arc of an ellipse, and becomes a straight line. The body thus moves uniformly across the hollow of the shell, and enters again on the opposite side, with the same velocity it had on quitting the shell. The central attraction of the shell begins to be felt as soon as a layer of thickness dr is trav- ersed, for the space 4.Trr-dr has a mass ^-Kcrr'-dr. and it attracts as if collected at the center of the shell. This force grows till the star emerges from the shell on the outside, when it is equal to that operating at the moment the star first entered the shell. Consequently it will depart from the shell on a Keplerian ellipse exactly similar to that on which it first came in ; and the total external orbit will consist of two ex- actly similar and similarly situated parts of ellipses, joined by straight lines in the hollow of the shell, and within each layer of the shell gradually passing from the arc of an ellipse to a straight line. This path is illustrated by the accompanying figure. The orbit here described supposes that no local perturbations have occurred during the complete revolution. Let us now consider the average effect of such perturbations as will occur. These may be best understood by analogy with the average effect of Jupiter on comets crossing his orbit. It is will known that many comets orig- inally traveling in orbits almost parabolic have been thrown within Jupiter's orbit, till quite a large family has been acquired with short Fig. 3. Illustrating the capture of an os- cillating star by the action of a spherical shell uniformly filled with stars as in a globular cluster. 146 SEE— DYNAMICAL THEORY [April 19, periods, and aphelia near Jupiter's path ; and those which still over- lap his orbit are being gradually worked into the more stable region within the orbit of that giant planet. In the same way the asteroids have been thrown within Jupiter's orbit, as H. A. Newton justly remarked in 1894 (cf. my "Researches," \^ol. II., 1910, p. 699), by a process which Professor E. W. Brown has more fully investi- gated in the Monthly Notices for March, 191 1. Professor H. A. Newton's researches and those of Callandreau and Tisserand on the capture of comets are well known, and need not be described here. Now if for Jupiter we substitute the action of the shell of the cluster, it may be thought that Jupiter is a very large mass, while the comets are very small ; whereas the stars in the shell of the clusters are not supposed to be so much larger than the star falling in. This is ver}' true, but as the shell contains many stars in mutual adjustment to an average state of stability, the oscillating star in the course of ages will be disturbed by the many stars, and the cumulative effects will be added together, just as the actions on comets are by the massive planet Jupiter. The mass of the shell greatly exceeds that of the single oscillating star, and even if some of the individual stars in the shell are considerably disturbed, yet the disturbance in successive revolutions will not effect the same stars, owing to movements within the shell of the cluster; and thus in the long run the only possible effect of the action of the many upon the one visiting star will be to dampen its energy of oscillation, till it too will have its path reduced and take its place in the shell with the original group. Thus the visitor from without is entrapped and its movements dragged down to the dead level of the rest of the stars in the shell. This is a general explanation of the capture process established by the more rigorous method of integration depending on Green's theorem, when some of the terms become infinite. It seemed desir- able to examine the matter from both points of view. To be sure this transformation may take many millions of years, but the average effect of the action of the shell in the long run is certain. As the stars in the shell are comparatively quiescent, the i9i-'.l OF THE GLOBULAR CLUSTERS. 147 only possible average effect of their action on the visitor will be to exert a drag on its motion. Some of the quiescent stars may be slightly disturbed by the passing body, but as the effect of one appulse is likely to be comparatively small, the stars in the shell will readjust the relations among themselves easily, while the visitor will suffer a considerable retardation of its oscillation. And after many appulses the visitor will have its motion restricted to the shell like the motion of the multitude of stars composing it. . This explains in a simple manner the capture process by which clusters are built up, and given such accumulation of density towards their centers. For the clusters are made up of a series of shells, and if the effect of one shell is of this type, the effect of all the shells will be an integration of these damping effects. It is no wonder therefore that all the clusters show such pronounced accumulation of density towards their centers. It is the inevitable outcome of this capturing of foreign bodies in the course of immeasurable time. In section III. we have admitted the possibility that defects in our photographs will account for the central density in clusters ex- ceeding that of the atoms in a globe of monatomic gas in convective equilibrium; but in view of this capture process, it seems much more likely that the stars are accumulating in these centers beyond the normal density for a mass of monatomic gas. Thus have the clus- ters been built up to such extraordinary accumulation that they justly excited the wonder of Sir William Herschel. XI. The Globular Clusters can be Explained Only by the Capture Theory. The figures of the clusters, nebulse and other sidereal systems impressed Herschel with the view that there is a clustering power in nature, everywhere gathering the stars into globular swarms, and moulding the nebulosity into figures of greater and greater sym- metry {PJiil. Trans., 1789, pp. 217-219). This is the earliest outline of the modern capture theory as applied to clusters and nebulse of symmetrical figure. It is evident that this process gives a good ex- planation of the origin of the clusters, and that they can be explained in no other way. 148 SEE— DYNAMICAL THEORY [April 19. It is obvious that masses of such vast extent and perfectly round figure and symmetrical arrangement of internal density, could not possibly have arisen by any of the theories of collision formerly held but now abandoned. For collisions could not disperse the stars to such great distances over spaces measured by many thousands of light years, nor could they give rise to the observed symmetrical arrangement of the parts. IMoreover, clusters embracing thousands of stars, if due to collision, would imply two equally immense masses in collision ; and there would be so few of these large masses in the universe, that it is inconceivable that they would ever come into col- lision. The whole collision doctrine is manifestly inconsistent with the symmetry and order found in the clusters, which can therefore be explained only by the capture theory, based on the expulsion of dust from the stars, and its collection from all directions into masses of impressive symmetry. This theory not only gives a perfectly satisfactory account of the phenomena of the clusters, which are wonderful in the extreme, and show steady and uniform processes working slowly over immeasur- able ages; but also establishes the theory itself by the way the most intricate and diverse phenomena are woven into a continuous whole. The first rule of philosophy laid down by Newton in the " Prin- cipia " is that: "Wc are to admit no more causes of natural tilings than such as are both trne and sufficient to explain their appearances." He explains this by adding that " philosophers say nature does noth- ing in vain, and more is in vain when less will serve." The next rule is that we are to ascribe the same natural effects to the same causes. If therefore the capture theory alone will explain the clusters, where the scale of the operations is immense, and the symmetry so perfect that other causes are easily excluded ; and on the other hand it will equally account for all other known phenomena of the sidereal universe, it follows from Newton's rules for philosophizing that this cause alone can be regarded as established. The definite proof of the capture theory for the formation of clusters and nebulae thus renders its operation general throughout the sidereal universe. Everywhere the large masses drift towards the most powerful neigh- boring center of attraction, while fine dust is expelled from the stars 191^.] OF THE GLOBULAR CLUSTERS. 149 to produce nebulae in the vacant regions of the heavens ; and this concentration of the large masses under gravity, and the redistri- bution of the fine dust by the action of repulsive forces is the great law of nature which preserves the order of the starry heavens. XII. The Mutual Interaction of Attractive and Repulsive Forces Confirmed by a Delicate Criterion Based on the Exact Equality of Thousands of Associated Stars in a Cluster. Elementary considerations on the principles of probability will show that the chances of even two associated stars being of equal brightness is slight ; it is still smaller for three, four and higher multiples, and when the number becomes large the probability of the chance association of such equal stars totally disappears. Accord- ingly, it is not by accident that thousands of stars observed in a cluster, with perfectly symmetrical accumulation towards the center of the associated stars, all known to be at nearly the same distance from us, are as exactly equal in every respect as the finest coins turned out of a mint. There must be in nature a reliable process for the manufacture of these nearly equal stars, which is described above for the first time. To prove this more conclusively we may compare clusters with double and multiple stars, which are systems of lower order. In binaries the components often are very unequal in brightness, and also in mass. The same principle, as is well known, holds for triple and quadruple stars. Now in these double and multiple star systems the ratio of the mass of the components depends on the chance division of the original nebulosity gathered from the heavens, not from the associated stars themselves; but in the clusters the principle of redistribution becomes largely predominant, owing to the great number of radiating centers in close association. It is not surpris- ing, therefore, that the lower orders of stellar systems should in- clude : first, single stars, with planetary systems, amounting to about four fifths of all the stars; second, binary stars, with unequal com- ponents ; third, multiple stars, also with components very unequal. This inequality of the associated stars is to be expected in all sidereal PROC. AMER. PHIL. SOC, LI. 204 G, PRINTED JUNE 6, I9I2. 150 SEE— DYNAMICAL THEORY [April 19, systems made up of a small number of bodies, but the visual double stars, as the brighter and more easily recognized systems, appear to have components more nearly equal than the much greater number of systems,* which remain invisible at the distance of the fixed stars. The association of thousands of equal stars in a cluster must therefore depend on something besides a chance distribution, or par- tition of the primordial nebulosity. For although the clusters are very far away, and the double stars in a cluster would thus appear single from the perspective effect of distance alone, yet the distance would not prevent fainter single stars from appearing on the back- ground of the cluster if they were present. Perrine points out in Lick Observatory Bulletin No. 155 that in cluster there is rarely a difference of more than two magnitudes among the stars com- posing it. This difference probably depends on difference in the spectral types, rather than on difference in mass. The conclusion that the great equality in luster depends on the essential equality in the redistribution of dust within the system therefore seems unavoid- able, as a necessary result of known laws of nature actually proved to be in operation. If therefore this argument regarding the origin of clusters, based on the equality of the stars, is admissible, the explanation may as confidently be depended on as the law of gravi- tation itself. For the testimony of the sidereal universe to its truth seems to be absolutely overwhelming. There are in all over one hundred globular clusters, and they include millions of stars; so that the observed order of nature obviously rests on a fundamental cause. Accordingly, if we admit the truth of this theory of clusters, which now seems to be well established, through the evidence pre- sented by hundreds of globular clusters, and by the analogous evi- dence offered by thousands of nebulae, we have at the same time an equally satisfactory proof of the universality of the operation of repulsive forces in nature. With his usual penetration Herschel saw in the accumulation of density and brightness towards the centers of these masses an incontestible proof of the existence of a clustering power operating throughout the sidereal universe. Now by exactly reversing his argument we have an equally valid proof of the operation of repulsive forces, to give the original distri- * Resembling planetary systems. 1912.] OF THE GLOBULAR CLUSTERS. 151 bution of dust, out of which the ckisters and nebulae are finally built. Moreover, as already remarked, this general argument, drawn from the sidereal universe as a whole, is minutely verified in the construc- tion of clusters, by the exact equality of thousands of closely asso- ciated stars, which thus supply a criterion of unrivaled rigor. This cluster criterion authorizes the conclusion that the theory may now be removed from the category of speculation and entered in the list of established facts relating to the physical universe. The most obvious indications of nature are plain enough ; and in interpreting them all we need to do is to follow the theory of probability, which, as Laplace has remarked, is nothing but common sense reduced to calculation. This theory tells us that there is a deep underlying cause for the perfect equality of the associated stars in clusters, which can be nothing else than the mutual interaction of attractive and repulsive forces in these island universes. XIIL The Real Dimensions of the Clusters and the Average Distances of the Stars Apart. The question of the distances of the clusters is one which at present cannot be fully answered, owing to the lack of certain obser- vational data; but it is well known that nearly all these masses of stars are very remote. To be sure such an outspread swarm as Coma Berenices, really is a cluster so near us as not to be suspected of belonging to the same type as the better defined Pleiades, Praesepe and Omega Centauri. But leaving out of account a few exceptions of this class we may say that the globular clusters in general, like the nebulae considered by Dr. Max Wolf in A. N., 4549, are thou- sands of light-years in diameter. This is proved by the comparative faintness of the component stars, and the large angular magnitude of the clusters as seen in the sky. Accordinglv, even when there are thousands of stars in a verv compressed cluster, they are not really close together, but separated by great intervals, of the order of a light-year. Thus the components in a dense cluster probably are somewhat closer together than our sun is to Alpha Centauri ; and yet the intervals can hardly be less than a ten thousand fold radius of the earth's orbit, the light-year 152 SEE— DYNAMICAL THEORY [April 19, being 63,275 times that distance. In fact the average distances are likely to be several light-years, and thus of the order 100,000 radii of the earth's orl)it. This great distance of the stars apart, even in the densest cluster, will enal)le us to realize the well-known fact that our sun is in a solar cluster, which includes Sirius, the stars of Ursa Major, and many other bright objects. It also enables us to appreciate why the motion in the clusters necessarily is slow, owing to the great inter- vening spaces and the feebleness of the disturbing forces acting on the individual stars. And at the same time we easily see why such a system, under the mutual gravitation of its parts, might survive for infinite ages, without sensible decay of its order or stability. Newcomb therefore was right when he remarked that there might be planets revolving about the stars in a cluster (article " Stars," Encyclopedia Americana) ; for we ourselves live on a planet attached to a star of the solar cluster, and the other clusters of the sidereal universe are not very different from that including our sun. Sir William Herschel was of the opinion (Phil. Trans., 1789, p. 225) that the clusters which are most compressed are drawing on towards a period of dissolution. In an earlier paper of 1785 Her- schel suggested that the clusters are the laboratories of the universe where the most salutary remedies for the decay of the whole are prepared (Phil. Trans., 1785, p. 217). In my "Researches," \"ol. II., 1910, I have independently pointed out that the condensation of very compressed clusters into one mass is the only logical explanation of such immense stars as Canopus and Arcturus. For it appears that with the advance of age the state of compression slowly increases, and when it has become extreme, and all the single bodies are drawn very near the center, it is quite likely that the cluster by conflagration may become the furnace of a labo- ratory of the universe for repairing through repulsive forces the ravages wrought by universal gravitation in the course of millions of ages. If this be true someone may ask why we do not find some cluster in the stage of conflagration? But if we recall that only a little over one hundred globular clusters are known, with their internal '9'-] OF THE GLOBULAR CLUSTERS. 153 spaces still large, and remember also the vast interval of time re- quired to produce the ijiz'isiblc state of close compression, it will become evident that the chances of our living at the epoch of a cluster conflagration totally disappears, and the most we can hope to recognize is the resulting giant star such as Canopus. XIV. Proof that ]\Iatter Actually is Lost from our Sun Supplied by the A^ery Straight Tails of Comets Devel- oped IN Close Perihelion Passage. In view of the recent development of the doctrine of repulsive forces in nature, it becomes important to have readily at hand specific illustrations of these forces adequate to meet any demand that may be made on the new doctrine. Now the tails of comets and the streamers of the corona, as explained by Arrhenius in Lick Observa- tory Bulletin 58, give abundant evidence of the operation of repulsive forces directed from the sun ; but every case does not show a repul- sion sufificientl)^ strong to carry the particles away from our solar system on parabolic or hyperbolic paths. The question thus arises : Are there any known cases of repulsion sufiiciently powerful to carry particles away from our sun to the other stars, and thus cause a secular decrease in the sun's mass? We may answer this question in the affirmative, for the following reasons : 1. Those comets which have had a very small perihelion distance, as the great comets of 1680, 1843 ^^'^ 1882, have all had also very straight tails, which were found by calculation to be of immense length near perihelion passage. It is well known that this extreme straightness of tail indicates very powerful repulsion of the particles composing it. 2. By actual calculation I have established the fact that the veloc- ity of the particles in the tails of the above comets, at perihelion, exceeded the parabolic velocity of a body driven away from the sun. The matter in these tails therefore was not only diffused over the solar system, but also carried away to other fixed stars. 3. Now if this repulsion with more than parabolic velocity could happen for vaporous matter developing in a comet's tail near peri- helion, but remaining of sufficient density and luminosity to be visible 154 SEE— DYNAMICAL THEORY [April 19, to the eye against the liackground of the sky, because it is condensed into a beam, the same thing- obviously could develop also for par- ticles in the solar corona itself, even if they be not sufficiently con- centrated to present at night the aspect of a ray extending from the sun. In fact such rays of charged matter are proved to emanate from the sun by Maunder's researches on the sun spots and magnetic disturbances noted at Greenwich, and published in the Monthly No- tices of the Royal Astronomical Society for 1905. 4. The emission of charged particles from the sun being thus clearly proved, the only question remaining open to discussion is whether any of the matter thus driven away from the sun goes away to the other fixed stars. But as my calculations show this to occur for the particles of the tails of comets which graze the sun's disc in perihelion— the only case in which the beams can be distinctly seen and the velocity of the particles determined from the lack of curva- ture in the tails — it must, by similarity of causes and effects, be held to occur also for some of the particles in the corona, even though they be invisible, owing to the diffuseness of the streamers. 5. The sun therefore is losing matter incessantly as well as gain- ing it, in the form of meteorites from celestial space. And in my "Researches," Vol. II., 1910, I have shown that the secular accelera- tion of the earth's motion indicates that at present the gain exceeds the loss; but if the sun was hotter in past ages, the reverse tendency formerly may have been at work. 6. Thus it appears to be demonstrated, by observed phenomena in our planetary system, that the sun is both gaining and losing matter, but that at present the rate of gain exceeds that of loss, so that there is a secular acceleration of the planets of such excessively minute character that it long escaped detection. In other fixed stars, it is probable that various combinations of gain and loss are at work ; and we may be sure that the masses of the stars are not strictly con- stant over long ages, however approximately an even balance of gain and loss may hold for shorter intervals of time. The view held by Newton and adopted by Lagrange and Laplace that -the sun's mass may be considered constant, is only approxi- mately true, and cannot properly be applied to the secular equations I9I2.] OF THE GLOBULAR CLUSTERS. 155 for the motions of the planets; and what has been found true of our sun, as respects a growth of mass, from the records of ancient ecHpses, will naturally be adopted for other solar stars, while a secu- lar decrease in mass may be assumed for some of the Sirian stars, owing to the intensity of their radiation. XV. The Building of Clusters and Nebula Condensed Towards the Center, as Illustrated by the Very Elongated Elliptic Orbits of our System of Comets. If we seek to inquire how clusters and nebulae much condensed towards the center are built up by the process of capture, we shall find the general mathematical treatment by Green's theorem already given very satisfactory, for large bodies of the type of stars. It is equally convincing mathematically as applied to small bodies of the type of comets, but it is perhaps well to notice how the comets de- scending to our sun in very elongated ellipses have served to supply material for building up the planets and sun. This remarkable system of comets, with elliptic orbits equally diffused in all directions about our sun, is a sure sign that the nebulosity now condensed into our comets came originally from the fixed stars. But if on the one hand, this equality of distribution of the aphelia in every direction points to the original entrance of the mate- rial into our nebula from without, the other equally remarkable prop- erty of high eccentricity, on the other, points to a similar conclusion. At the same time this coming in of matter from a distance makes possible the growth of the planets near the center of the system, because near perihelion the comets often pass so close to the planets as to have their orbits transformed, and their masses disintegrated and their dust absorbed by the planets. It is by moving against the resistance due to comets, and meteor swarms that the planetary orbits have been rendered so perfectly circular that the Greeks be- lieved that the Deity had chosen the circle for the paths of the planets, because the circle was held by the ancient geometers to be a perfect figure. Now what takes place about our sun, in the solar cluster, may 156 SEE— DYNA^IICAL THEORY [April 19, also take place, in other star clusters of the Alilky Way. There are in every region systems of bodies corresponding to our comets; and as they travel in very elongated ellipses, they tend to build up the bodies near the centers about which they revolve. In this way there must be countless infinities of comets working in towards the centers of the globular clusters ; and thus they build up the equality of the stars in these regions, while at the same time the increase of mass and the resistance to orbital motion thus arising tend to round up the cluster and give increasing density towards the center. Thus the analogy of the comets revolving in very elongated orbits and being destroyed to build up the planets and the sun, will also hold in the building up of a cluster. Not only may mature stars be cap- tured and adjusted to the average oscillation within a cluster, but also myriads of millions of comets ; and it is in this way largely that the cluster augments in mass and density towards the center. This growth of central power in turn augments the condensation observed in the clusters, and tends still further to produce a secular decrease in volume; just as the planets are drawn nearer the sun by the increase of the sun's mass. The shrinkage in the volume of a cluster is thus analogous to the diminution of the dimensions of the primi- tive orbits of the planets. And just as the planets in time will fall into the sun, so also will the stars of a cluster eventually combine into one great central star and thus produce an Arcturus or a Canopus. The study of the system of comets about the sun, and the way the planets have been built up near the center of the solar nebula, thus gives us much light on the central accumulations noted in globular clusters. The smaller masses drawn in from without tend to augment the central bodies of the system ; and this growth of mass in turn produces a further condensation of the original group, whether it be a planetary system, or a globular cluster of the highest order of glory and magnificence. '9I5-] OF THE GLOBULAR CLUSTERS. 157 XVI. The Projectile Forces which Set the Double and Mul- TIPPLE Stars Revolving in Their Orbits, Point to Origin in the Distance. If we have a stellar system made up of several components, we may designate the masses of the individual stars by M^, M,, M^ . . ., Mn. We shall first consider a binary star with masses M^ and M,. Then the moment of momentum of the components about the com- mon center of gravity of the system will be m^ + mXm^ + m/'-^^' )■ (50j ( ^^P \r^ / 2 ^^1^2 2n / -2 where c is the eccentricity of the orbit, and p the radius vector, and n the mean angular velocity in the orbit (cf. inaugural dissertation, "Die Entwickelung der Doppel-Stern Systeme," Berlin, 1892, p. 16). When the other elements are unchanged, we find that the moment of momentum of the binary system decreases with the increase of the eccentricity. In case of a circular orbit, e vanishes, and O is con- stant. In the general equation of the planetary theory the unit of time may be so chosen that the constant of attraction (cf. Gauss, " Theoria Alotus," Lib. I., § i ) becomes and we may therefore put Vt for n and p for a, and the second mem- ber of (50) becomes p-Q.Vi-e' = -,r^,^-^.^.p^V\-c-, (52) the radical involving e to be unity in circular orbits. From this equation (52) it appears that with constant mass the moment of momentum of a system of double stars depends on the square root of the mean radius vector, and therefore increases rap- idly with the distance. 158 SEE— DYNAMICAL THEORY [April 19, Other conditions being equal, the maximum moment of momen- tum would therefore be attained by the separation of two stars to a great distance, yet a pair of such passing stars would have to have peculiar directions and velocities to enable them under mutual gravi- tation to form a system. If the motions of two stars were directed towards the same point in space, and with velocities which would enable one to overtake the other, before or after the point was reached, one might revolve about the other ; and with proper relative velocity — to be gotten either by altering the directions of motion, or by adjusting the velocities in the converging lines of motion — the two stars might form a binary system. This dynamical condition of formation is so difficult to realize in practice that we may be sure that it is quite rare in nature ; and that the vast m.ajority of double stars have developed from nebulae, by the appropriate division of the elements between two leading centers of condensation. But it is now recognized that the nebulae them- selves have developed from dust expelled from the fixed stars and were originally of vast extent; and hence even if the bodies into which they condense gradually approach the center of gravity of the system, as the stars increase in mass and revolve against the nebular resisting medium and their orbits grow smaller and smaller and rounder and rounder, it will yet follow that many double stars have components so far apart that their systems have large moments of momentum of orbital motion. The difficulty of explaining the large orbital moments of momen- tum of double stars first arose in completing certain calculations for my inaugural dissertation at the University of Berlin just twenty years ago. At that time I saw that a wide separation of the compo- nents of a system gave large moment of momentum, and that in order to account for the orbital moment of momentum by the hypoth- esis of tidal friction first developed by Sir George Darwin and after- wards extended by me to binary systems, it was necessary to endow the stars with very rapid axial rotation. Otherwise the mean dis- tance of the components would not be greatly increased by the ex- haustipn of the moments of momentum of axial rotation under the secular action of tidal friction. I9I2.] OF THE GLOBULAR CLUSTERS. 159 At this early stage in the study of the problems of cosmogony, naturally I had not exhausted the other possible modes of formation, though I had largely excluded the capture of single stars by chance approach due to difference in proper motion. The further study of this problem has occupied a part of the past twenty years, but as it has now led to the establishment of a great law of nature, one may feel that the labor has not been in vain. From the above reasoning it will be found : 1. That if the globes of the stars of a binary be expanded till a hydrostatic connection is established between the components, the fluid will thereby become so rare that no hydrostatic pressure could be exerted to throw oft" a companion by rotation. 2. A rotation rapid enough to produce such a separation could not be accounted for by natural causes. 3. Hence it is clear that the premise implying a separation by rotation is false; and the true mode of formation is diametrically opposite to what was long believed. Instead of being thrown oft' by rapid rotation, the attendant bodies have all been formed in the dis- tance, and added on from without, so that they have neared the centers about which they now revolve. This uniform law greatly simplifies all our conceptions of cosmical evolution. To illustrate the relative significance of the moments of momen- tum of the axial rotations compared to the moment of momentum of orbital motion, it suffices to cite the case considered in my inau- gural dissertation of 1892, pp. 37-38. In this case each of the two equal stars imagined expanded into a nebula has three times the mass of the sun ; and the axial rotations are such as to give an oblateness of 2/5. The stars are set in motion at a mean distance of 30 astronomical units. In the special units there adopted, it turns out that the mo- ments of momentum of the axial rotations have the numerical values 0.394, or 0.788 for the two stars; and the moment of momentum of orbital motion becomes 2.378. Thus with the two stars so far apart as 30, it is impossible to keep the figures of equilibrium stable and yet give them rotations rapid enough to render the moments of momentum of axial rota- tion large compared to that of the orbital motion. Nevertheless, a 160 SEE— DYNAMICAL THEORY [Ai>rii 19, double star orbit with a mean distance of 30 must be considered small compared to many orbits which exist in the heavens. For there are physically connected stars which show very little motion in a cen- tur}-, and others which remain (juite fixed, as may be clearly estab- lished by comparing modern measures with those of Herschel and Struve. The conclusion from this calculation is that the observed mean distance of wide double stars has not been developed by the transfer of moment of momentum of axial rotation to moment of momentum of orbital motion. By such transfer of moment of momentum the orbit may indeed be expanded, but not to many times its original size. On this tidal frictional theory the larger orbits of double stars could not be explained satisfactorily. The difficulty encountered some twenty years was therefore first overcome in developing the second volume of my " Researches," along the lines of thought result- ing from the extension of Babinet's criterion in 1908. Looking at the problem in the light of recent progress it is evident that the large and highly eccentric orbits of double stars do undoubt- edly point to capture ; that is, the formation of separate nuclei at a great distance, and the revolution of the two stars in narrowing orbits about the center of gravity of the system. If this process of revolution in the original nebula should continue long enough, the size and eccentricity of the orbit would be much reduced ; and we should thus obtain systems of the type commonly observed to be in comparatively rapid revolution. There is thus established a real connection between the revolving visual double stars and the much larger number of physical systems which have remained nearly if not quite fixed since the epoch of Herschel and Struve. This inference is also sustained by recent progress in double star astronomy, which shows that the longer the period the higher the eccentricity, and the same tendency holds for the rapid spectroscopic binaries, as I pointed out in 1907 {Monthly Notices, Roy. Astron. Soc, Nov., 1907). This unbroken continuity among all the classes of double stars shows that the cause is everywhere the same. If therefore the wdder visual double stars have formed from separate nuclei, in the condensing nebul?e, the explanation becomes valid also T9I2.] OF THE GLOBULAR CLUSTERS. 161 for the spectroscopic binaries; and the law of formation is the same for all the double stars as for the planets of the solar system, where Babinet's criterion is absolutely decisive against the detachment theory generally held since the days of Laplace, but now universally abandoned. Summary and Conclusions. Without attempting in this closing summary to recapitulate the contents of this memoir in detail, it may yet be well to draw attention to some of the most significant conclusions at which we have arrived. 1. As intimated in the first section of this paper the problem of ■w-bodies, under ideal dynamical conditions, remains forever beyond thepower of the most general methods of analysis; but the dynamical theory of clusters gives us the one secular solution of this problem found under actual conditions in nature. For when ii is of the order of 1,000, so as to give rise to a cluster, the clustering power observed by Herschel operates to exhaust the mutual potential energy of the system, and bring about increasing accumulation in the center, so that the cluster finally unites into a single mass of enormous magni- tude. Probably the giant stars of the type of Canopus and Arcturus have arisen in this way. 2. And since attendant bodies of every class — as satellites, planets, comets, double and multiple stars — tend everywhere to approach the centers about which they revolve, as an inevitable effect of the growth of the central masses and of the action of the resisting medium over long ages, it follows that the secular solution of the problem of clus- ters is more or less valid for all cosmical systems. They finally end by the absorption of the attendant bodies in the central masses which now govern their motions. 3. The dynamical theory of globular clusters shows that the clus- tering power inferred by Herschel is nothing else than the action of universal gravitation ; and that it operates on all sidereal systems, but does not produce the cumulative effect which Herschel ascribed to the ravages of time inside of millions of ages. 4. The globular clusters are formed by the gathering together of stars and elements of nebulosity from all directions in space; and 162 SEE— DYNAMICAL THEORY [April 19, this points to the expulsion of dust from the stars of the !\Iilky Way, and its collection about the region of the formation in such manner as to give essential symmetry in the final arrangement of the cluster, which doubtless has some motion of rotation, and originally a tend- ency to spiral movement. 5. The stars and smaller masses are captured by the mutual action of the other members of the cluster, and worked down towards the center of the mass. This gives a central density in excess of that appropriate to a sphere of monatomic gas in convective equilibrium (^. //., 4053, and .^. A^, 4104). 6. The density of the clusters is greater on the outer border than in a globe of monatomic gas, which shows that stars are still collect- ing from the surrounding regions of space. The starless aspect of the remoter regions about clusters is an effect of the ravages of time, as correctly inferred by Herschel in the course of his penetrating sweeps of the starry heavens. 7. And just as clusters under the mutual gravitation of the com- ponent stars contract their dimensions, with time, chiefly owing to the growth of the central masses, so also do other systems, whether the mass-distribution be single, giving a system made up of a sun and planets, or double, triple and multiple, giving binary, triple or multiple stars, or sidereal systems of still higher order. The tend- ency everywhere is from a wider to a narrower distribution of the large bodies ; while the only throwing off that ever occurs is of par- ticles driven away from the stars by the action of repulsive forces. 8. The orbits of the stellar and planetary systems are decreased by the growth of the central masses and rounded up by the action of the nebular resisting medium. And in like manner all clusters tend to assume spherical or globular figures, so as to justify the ex- pression of Plato, that the Deity always geometrizes; or Newton's remark that the agency operating in the construction of the solar system was " very well skilled in mechanics and geometry." 9. Newton required the intervention of the Deity to give the planets revolving motion in their orbits, because in the absence of repulsive forces he could not account for the dispersion of the matter, so as to produce the tangential motions actually observed. By means I9I2-] OF THE GLOBULAR CLUSTERS. 1(33 of the theory of repulsive forces, however, it is now possible to explain these projectile motions, which Herschel likewise pointed to as the chief agency for the preservation of sidereal systems. The only assumption necessary is an unsymmetrical figure of the primor- dial nebula, giving a whirling motion about the center as the system develops ; and since the dust gathers from all directions it is certain that this lack of perfect symmetry will nearly always develop, as we see also by the spiral nebulae. 10. It is this unsymmetrical form of the spiral nebulae produced by the gathering of the dust from the stars, or the slight relative tangential motion of stars formed separately but finally made to revolve together as a binary system, that gives the binary stars the projectile forces, with which they are set revolving in their orbits. In no case have they resulted from the rupture of a rotating mass of fluid under conditions of hydrostatic pressure as formerly believed by Darwin, Poincare and See. 11. Even if the rotation could become rapid enough to produce a separation, under conditions of hydrostatic pressure, by rupture of a figure of equilibrium, there would still be the equal or greater difficulty of explaining the origin of the primitive rapid rotation. This last difficulty escaped notice till we came to assign the cause of rotations, and found that mechanical throwing ofif was impossible under actual conditions in nature. It is therefore recognized, from the definite proof furnished by Babinet's criterion in the solar sys- tem, that such a thing as a throwing off never takes place; but that all planetary and stellar bodies are formed in the distance, and after- wards near the centers about which they subsequently revolve. 12. TJiis gives us a fundamental laiv of the firmament — tht^ planets being added on to the sun, the satellites added on to their planets, the moon added on to the earth, and the companions added on to the double and multiple stars — which is nozv found to be beau- tifully confirmed by the dynamical theory of the globular clusters. It is not often that such a great lazv of nature can be brought to light, ami it is zvorthy of the more consideration from the circumstance that it explains all classes of stellar systems by a single general principle. 164 SEE— DYNAMICAL THEORY [April 19. 13. As sidereal systems of lower order are conserved by projec- tile forces, it is probable that the clusters likewise' have a spiral motion of rotation, with similar projectile forces tending to counter- act simple progressive collapse. The period of the orbital revolution of the stars of a cluster is found to be common to all, without regard to the dimensions of the elliptical orbits described, and thus the whole system may have a common period of oscillation, after wdiich the initial condition is perfectly restored. This possibility in the dynamics of a cluster is exceedingly wonderful, and results from the central attraction depending directly on the distance. 14. The equality of brightness in star clusters shows that some process of compensation between the attractive and repulsive forces has produced stars of wonderful uniformity of luster. Thus the present investigation confirms the previous researches on the evolu- tion of the stellar systems, which have laid the foundations for a new science of the starry heavens. 15. Accordingly the capture theory of cosmical evolution being now firmly established for the clusters, where the nature of the process is entirely clear, it becomes at once a guide to us in dealing with systems of lower order ; and we see that the law of nature is uniform and everywhere the same, the large bodies working in towards the centers of attraction, while the only throwing off that ever takes place is of small particles driven out of the stars by the action of repulsive forces. All planetary bodies are formed in the distance, and have their orbits reduced in size by increase of the central masses, and rounded up by moving in a resisting medium. This is a perfectly general law of the sidereal universe. It verifies the early conjectures of Plato and Nezvton as to the stability of the order of the world, and shoics that these ilhistrious philosophers were quite justified in concluding that the Deity alzi'ays geometrizes. The spiral nebulae tend to develop systems with rounder and rounder orbits, and the clusters made up of thousands of stars assume globular figures with minimal surfaces and internal density so arranged as to give maximum exhaustion of the potential energy. 16. This is geometry of the most marvellous kind, as we find it impressed on the systems of the sidereal universe ; and the perfection '91-'-] OF THE GLOBULAR CLUSTERS. 165 of this most beautiful science of celestial geometry may be consid- ered the ultimate object of the labors of the astronomer. The philosophic observer is not and never can be content with mere ob- servations of details which do not disclose the living, all-pervading spirit of nature. 17. If, then, the mystery of the gathering of stars into clusters is now penetrated and traced to the clustering power of universal grav- itation, so also is the mystery of the converse problem of starless space, which was a subject of such profound mediation by the great Herschel. 18. This incomparable astronomer likewise correctly concluded that the breaking up of the Milky Way into a clustering stream is an inevitable effect of the ravages of time ; but we are now enabled to foresee the restorative process, under the repulsive forces of nature, by which new nebulae, clusters and sidereal systems of high order eventually will develop in the present depopulated regions of starless space. 19. If there be an incessant expulsion of dust from the stars to form the nebulae, with the condensation of the nebulae into stars and stellar systems, while the gathering of stars drawn together by a clustering power operating over millions of ages gives at length a globular mass of thousands of stars accumulating to a perfect blaze of starlight in the center, but surrounded externally by a desert of starless space resulting from the ravages of time, certainly the building of these magnificent sidereal systems may well engage the attention of the natural philosopher. 20. The foremost geometers of the eighteenth century, including Lagrange, Laplace and Poisson, were greatly occupied with the problem of the stability of the solar system ; and in his historical eulogy on Laplace the penetrating Fourier justly remarks that the researches of geometers prove that the law of gravitation itself operates as a preservative power, and renders all disorder impos- sible, so that no object is more worthy of the meditation of philoso- phers than the problem of the stability of these great celestia' phenomena. But if the question of the stability of our single planetary system PROC. AMER.?PHIL. SOC, LI. 2O4 H, PRINTED JUNE 7, I9I3. 166 SEE— DYNAMICAL THEORY [April 19, may so largely absorb the talents of the most illustrious geometers of the age of Herschel, hozv much more justly may the problem of the stability of clusters, involving many thousands of such systems, claim the attention of the modem geometer, zvho has zvitnessed the perfect unfolding of the grand phenomena first discovered by that unrivaled explorer of the heavens f The grandeur of the study of the origin of the greatest of side- real systems is worthy of the philosophic penetration of a Herschel ! The solution of the dynamical problem presented surpasses the powers of the most titanic geometers, and would demand the in- ventive genius of a Newton or an Archimedes ! Yet notwithstanding the transcendent character of the problem, and the hopelessness of a rigorous solution in our time, even an imperfect outline of nature's laws may aid the thoughtful astron- omer, in penetrating the underlying workings of the sidereal uni- verse, and thus enable him to perceive the great end subserved by the development of the cosmos. If so, he may well rejoice, and ex- claim with Ptolemy: " Though but the being of a day, When I the planet-paths survey, My feet the dust despise ; Up to the throne of God I mount And quaff from an immortal fount The nectar of the skies." Starlight on Loutre, Montgomery City, Missouri, February 19, 1912. THE CLASSIFICATION OF THE BLACK OAKS. By WILLIAM TRELEASE. {Read April 19, igi2.) (Plates X-XIII.) Since Alphonse de Candolle^ pointed out that the abortive ovules occupy a definite position in a mature acorn, constantly basal or nearly so in some species and as constantly apical or nearly so in others, and crystallized the knowledge that the ripening of the fruit occurs in one season in some and requires two seasons in others (attending correspondingly retarded fertilization-) with as great constancy,^ so many other correlations in wood, bark, leaf, stamens and styles have been associated with these differences that the white oak and black oak groups* have long been recognized as presenting a natural division of our native species : the former with basal ovules, short styles with dilated stigmas, usually annual often stalked fruit essentially glabrous within and often with tuberculate or aristate cupule-scales, leaf lobes not bristle-tipped, pale often flaky bark and tough compact rather pale wood of slow growth ; the latter with apical ovules, elongated slender styles, usually biennial nearly sessile fruit tomentose within and rarely with tuberculate or tapered cupule- scales, bristle-pointed leaf lobes, dark often deeply checked but not flaking bark and darker wood of twice as rapid growth on the average. The principal doubts as to the sufificiency of these group charac- ters may be said to rest on an occasional easily understandable but none-the-less misleading slip of the pen such as that of de Candolle's ^A. de Candolle, Ann. Sci. Nat., Bot., IV., 18: 51. 1862. For various other places of publication in French and English, reference may be made to the catalogue of the Royal Society. * Conrad, Bot. Gac, 29 : 410. 1900. *A. de Candolle, /. c, 50. * Engelmann, Trans. Acad. Sci. of St. Louis, 3: 374, 381, 388. 1876-7; " Bot. Works," 390, 394, 397. 167 1G8 TRELEASE— CLASSIFICATION OF BLACK OAKS. [April 19, translator^ and of Professor Sargent,*' making the ovules appear to be basal in the black oaks ; and on puzzling facts as well as observa- tions on the dwarf live oaks, particularly 0. Emoryi which Engel- mann' and Greene* have treated as a black oak on its general assem- blage of characters, and Sargent^ (as did Engelmann^° at first) places with the white oaks because of its basal ovules. Without attempting a critical analysis of hybrids, segregates and aberrants, the present communication ofifers what appears to be a natural grouping of our black oaks, which have been arranged in floras and monographs usually and diversely in sequence dictated by convenience of foliage contrast — that is, descriptively rather than taxonomically. The classification here proposed was adopted some months since when the oaks growing about St. Louis were selected to illustrate to a university class the synthesis of generic concepts out of specific characters. This local flora is fairly rich in representation of Quercus, for its dozen species constitute about two-thirds of those of Missouri, half of those of the northeastern states, a fourth of those of the United States, and a twentieth of those of the world. For this rea- son it has been comparatively easy to extend the conclusions based on the local species so as to embrace all of those occurring east of the great plains — which are evidently of a common stock. The few species occurring between the continental divide and the desert, and the few found west of this natural barrier, appear to represent groups more properly coordinated with the entire assemblage of eastern species than with the sets into which this is divided. In them, perhaps, is to be found the key to an understanding of the history of the genus as it is now represented in North America. Not many words are needed to indicate the striking collective dif- ferences in bud and fruit between the three groups, black oaks, scarlet oaks and swamp oaks of the eastern states, as pictured in the accom- °A. de CandoUe, Trans. Edinburgh Bot. Soc, 7: 440. 1863. " Sargent, " Manual, Trees of N. A.," 227. 1905. ' Engelmann, /. c, 388, 394. ' Greene, " 111. of W. A. Oaks," 45. 1889. 'Sargent, /. c, 230, 286. '" Engelmann, /. c, 381-2. I9I2.] TRELEASE— CLASSIFICATION OF BLACK OAKS. 169 panying plates: the first (PL X.) with large hairy buds and rather large fruit with coarse cup-scales, the second (PI. XL) with medium- sized nearly smooth buds and moderate or large fruit with rather closer or finer scales, and the third (PI. XII.) with still smaller buds and acorns, these with still closer and finer cupule-scales. That the groups are closely allied is to be expected, and in bud and cup char- acters Q. coccinea connects the first two ; but a glance at the plates will show how distinct the collective impression produced by each group is, and how far from natural it is to place Q. marilajidica (PI. X., f. i) next 0. nigra (PI. XII., f. 2) because of a compara- bility in leaf shape that has worked mischief in the names both have borne, or Q. pahistris (PI. XII., f. i) next Q. rubra (PI. XL, f. 5) or O. vchitina (PI. X., f. 4), or to separate O. Catesbcci (PI. X., f. 2) far from 0. digitata (PI. X., f. 3) or even Q. marUandica, as is commonly done. An interesting feature in the cup of these latter species is that the scales are inflexed around its margin — com- monly in the first, occasionally in the others — a character to be con- nected with Engelmann's observation^^ that the tips of the leaf lobes are bent in in vernation in Catesbcci, though it is not absolutely lim- ited to them. Though homogeneous in external bud and fruit characters, the group of swamp oaks is subdivisible into a series with broad-lobed leaves, the water oaks, in which the leaves are flatly imbricated in the bud as in the black and scarlet oaks, and a series with narrow entire leaves, the willow oaks, in which the leaves are revolute in the bud — strongly so in Q. imbricaria, 0. Phcllos, Q. latirifolia and Q. pwnila; less rolled in Q. cinerea and Q. myrtifolia, and thus approaching the western groups, though the fruits of the two are very dififerent. Such Mexican bristle-leaved oaks as Q. Grabami are evidently of this general stock. Grouped primarily according to the characters here selected rather than leaf form, these oaks fall into line as follows: Black Oaks. Quercus marUandica (black jack). Quercus Catesbcci (turkey oak). " Engelmann, /. c, 376. 170 TRELEASE— CLASSIFICATION OF BLACK OAKS. [April 19. Quercus digitata (Spanish oak). Quercus vehitina (quercitron). Scarlet Oaks. Quercus coccinea (scarlet oak). Quercus ellipsoidalis (Hill's oak), Quercus rubra (red oak). Quercus texana (Texas red oak). Quercus nana (bear oak). Swamp Oaks. Water oaks. Quercus palustris {\i'm 02^^). Quercus nigra (water oak). Quercus georgiana (Stone Mountain oak). Willow oaks. Quercus imbricaria (shingle oak). Quercus Phellos (willow oak). Quercus laurifolia (laurel oak). Quercus pumila (running oak). Quercus brevifolia (cinnamon oak). Quercus myrtifoHa (myrtle oak). Olive Oaks. Quercus hypoleuca (white-leaf oak). Quercus Enioryi (Emory's oak). Holly Oaks. Quercus agrifolia (evergreen oak). Quercus Wisliseni (highland oak). Quercus calif ornica (Kellogg's oak). I9I2-] TRELEASE— CLASSIFICATION OF BLACK OAKS. 171 EXPLANATION OF PLATES. In all, the buds are enlarged three diameters, and the acorns and cu- pules are of natural size. No special care has been taken in the selection of material, except to get mature winter buds because the differences are less evident while they are developing, and to pick out average fruits from the varying assemblage presented by each species. Plate X. Black Oaks. — i, Qiiercus marilandica ; 2, Q. Catesbcci; 3, Q. digitata; 4, Q. velntina. Plate XI. Scarlet Oaks. — i, Qiiercus coccinea; 2, Q. ellipsoidalis ; 3, Q. texana (the northern form known also as Q. Schneckii) ; 4, Q. texana (from Texas) ; 5, Q. rubra; 6, Q. nana. Plate XII. Swamp Oaks. — Water Oaks: i, Querciis palustris; 2, Q. nigra; 3, Q. georgiana. Willow Oaks : 4, Quercus imbricaria; 5, Q. Phellos; 6. Q. laiirifolia; 7, Q. pumila; 8, Q. brevifolia; 9, Q. myrtifolia. Plate XIII. Western Black Oaks. — Olive Oaks : i, Quercus hypoleuca; 2, Q. Emoryi. Holly Oaks : 3, Quercus agrifolia; 4, Q. Wislizeni; 5, Q. cali- fornica. MAGELLANIC PREMIUM Founded in 1786 by John Hyacinth de Magellan, of London 191 2 THE AMERICAN PHILOSOPHICAL SOCIETY Held at Philadelphia, for Promoting Useful Knowledge ANNOUNCES THAT IN DECEMBER, 1912 IT WILL AWARD ITS MAGELLANIC GOLD MEDAL TO THE AUTHOR OF THE BEST DISCOVERY, OR MOST USEFUL INVENTION, RE- LATING TO NAVIGATION, ASTRONOMY, OR NATURAL PHILOSOPHY (mERE NATURAL HISTORY ONLY EXCEPTED) UNDER THk FOLLOWING CONDITIONS : 1. The candidate shall, on or before November i, 1912, deliver free of postage or other charges, his discovery, invention or improvement, addressed to the President of the American Philosophical Societj, No. 104 South Fifth Street, Philadelphia, U. S. A., and shall distinguish his performance by some motto, device, or other signature. With his discovery, invention, or improvement, he shall also send a sealed letter containing the same motto, device, or other sig- nature, and subscribed with the real name and place of residence of the author. 2. Persons of any nation, sect or denomination whatever, shall be ad- mitted as candidates for this premium. 3. No discovery, invention or improvement shall be entitled to this premium which hath been already published, or for which the author hath been publicly rewarded elsewhere. 4. The candidate shall communicate his discovery, invention or improvement, either in the English, French, German, or Latin language. 5. A full account of the crowned subject shall be published by the Society, as soon as may be after the adjudication, either in a separate publication, or in the next succeeding volume of their Transactions, or in bothi 6. The premium shall consist of an oval plate of solid standard gold of the value of ten guineas, suitably inscribed, with the seal of the Society annexed to the medal by a ribbon. A.11 correspondence in relation hereto should be addressed To THE Secretaries op the AMERICAN PHILOSOPHICAL SOCIETY No. 104 South Fifth Street PHILADELPHIA, U. S. A. General Index to the Proceedings OF THE American Philosophical Society Volumes 1-50 (1838-1911) Just Published Pricey One Dollar TRANSACTIONS M OF THE American Philosophical Society HELD AT PHILADELPHIA For Promoting Useful Knowledge New Series, Vol. XXII, : Part /, ^/c, J J pages. (Recently Published.) One hundred and seventy-five Parabolic Orbits and other Results deduced from over 6300 Meteors. By Charles P. Olivier Subscription — Five Dollars per Volume Separate parts are not sold Address The Librarian of the AMERICAN PHILOSOPHICAL SOCIETY No. 104 South Fifth Street PHILADELPHIA, U. S. A. PROCEEDINGS OF THE American Phil(;)$9|]f|;ifc Society HELD AT PHILADELPHIA FOR PROMOTING USEFUL KNOWLEDGE Vol. LI. July, 191 2. No. 205. CONTENTS. Heredity of Feeble -raindedness. By Henry H. Goddard 173 The Heredity of Epilepsy Analyzed by the Mendelian Method. By David Fairchild Weeks 178 Is the Control of Embryonic Development a Practical Problem ? By Charles R. Stockard 191 An Avian Tumor in its Relation to the Tumor Problem. By Peyton Rous, M.D : 201 The Protein Poison. By Victor C. Vaughan, M.D 206 Some Geochemical Statistics. By Frank Wigglesworth Clarke 214 Thermal Relations of Solutions. By William Francis Magie 235 New Magnetic Charts of the Indian Ocean. By L. A. Bauer 240 The Dairy of a Voyage to the United States, by Moreau de Saint-Mery. By Stewart L. Mims 242 The Classification of Carbon Compounds. By Marston Taylor Bogert. , . 252 Stated Meeting, April 12, igi2 ix General Meeting, April 18, ig and 20, igi2 x Stated Meeting, May j, igi2 xvi PHILADELPHIA THE AMERICAN PHILOSOPHICAL SOCIETY 104 South Fifth Street 1912 CORRIGENDA. In Vol. LI, No. 203, Dr. T. J. J. See's paper on the Depth of the Milky Way ; page 12, 8th line from topp^^r, jliarge read small ** ** loth ** ** " ** decreasing r^alJlS0li55 Fig. 3. The central mating in this case is that of a feeble-minded man and an epileptic woman. The man had an epileptic brother, who in turn had a feeble-minded son, while the woman came from an insane mother and had a feeble-minded uncle. There were six children; the first died in infancy, the second and fourth were feeble-minded, the third was epileptic, the fifth is a feeble-minded boy, who is at The State Home for Boys, while the last is also feeble-minded, and he is cared for at a Children's Industrial Home. The mother and father are dependent on the town for support, the mother's mother died in the State Hospital for the Insane. This mating is of the type nuUiplex X nuUiplex. E, epileptic; F, feeble-minded; /, insane; A, alcoholic; N, normal. Case 4,369. related, thus connecting their pedigree with others already acquired, so that only 381 different families are involved in our study. The frequency with which the same name occurs on many of the charts indicates that there is little doubt but that future study will determine their relationship and show some of these to be of the same blood. The total number of epileptics recorded on the charts was 756, which was 3 per cent, of the total chart population of 21,558, or 9 per cent, of the 8,698 classified individuals. 182 WEEKS— HEREDITY OF EPILEPSY [April 19, In analyzing our data, we have classed it under the six kinds of matings, as follows : NULLIPLEX X NULLIPLEX. There are twenty-seven fraternities in which both parents are either epileptic or feeble-minded; 16 of these matings are principal matings and 11 secondary matings. In three of the matings both of the parents were epileptic. Of the 28 conceptions, two were stillbirths, 3 miscarriages, 3 died before Q O Q-r4& AT up li] E © 0 <®Sl (§m (§M a Fig. 4. This chart shows the offspring in a case where both the father and mother were feeble-minded; the father was alcoholic and died of tuber- culosis, while the mother was sexually immoral and was the illegitimate child of a feeble-minded woman. There were seven children; one, the sixth, is thought to be by a dififerent father; of the others five are feeble-minded and one is epileptic. After the father's death the mother married a feeble-minded man, who is the younger brother of her daughter's feeble-minded husband. E, epileptic; F, feeble-minded; A, alcoholic; T, tubercular; Sx, sexually immoral; A^, normal; ■ — , illegal union. Case 3,037. two years of age, and one (an infant) is too young for classification, leaving 19 about whom something definite is known. Of these, 8 were epileptic, 3 feeble-minded, and 8, who came from parents who developed epilepsy late in life, were tainted. (Fig. i.) In -fifteen fraternities in which one parent is epileptic and the other feeble-minded, there were 81 conceptions; 7 were too young I9I2.] ANALYZED BY THE MENDELIAN METHOD. 183 to be classified, and 19 died before 14 years of age. Of the 55 clas- sified, 29 were epileptic, 26 feeble-minded and i insane. (Figs. 2 and 3.) In nine fraternities in which both parents were feeble-minded, there were 56 conceptions. Of these, 4 died before two years of age, 14 were too young for classification. Of the other 38 of whom something definite is known, 7 were epileptic, 28 feeble-minded and 2 drunkards, who may or may not have been feeble-minded. (Fig. 4.) IS-rOI3-T-0^ I&-r-0 W-^r-^ doOOt}6C)66