_ cefnal ang Bietscc Oe . 4) O@GIEE Or ON at 1983. PARTS 1. andi? (Nos, 325 and 326) Poblished by the Society PAO wos NET, PS We 2008 hssmed Atigust, $983 ISSN 0035. = 9173 THE ROYAL SOCIETY OF NEW SOUTH WALES Patrons — His Excellency the Right Honourable Sir Ninian Stephen, A.K., G.C.M.G., G.C.V.O., K.B.E., K.St.J., Governor-General of Australia. His Excellency Air Marshal Sir James Rowland, K.B.E., D.F.C., A.F.C., Governor of New South Wales. President — Dr R.S. Vagg Vice- Presidents — Professor T. W. Cole, Dr G. S. Gibbons, Mr M. J. Puttock, Professor B. A. Warren Hon. Secretaries — Mr E. K. Chaffer Mrs M. Krysko v. Tryst (Editorial) Hon. Treasurer — Dr A. A. Day Hon. Librarian — Mr J. L. Griffith Councillors — Dr R. S. Bhathal, Mr D. S. King, Associate Professor J. H. Loxton, Associate Professor D. H. Napper, Dr F. L. Sutherland, Mr M. A. Stubbs-Race, Dr W. J. Vagg New England Representative — Professor S. C. Haydon Address:— Royal Society of New South Wales, PO Box N112 Grosvenor Street, NSW 2000, Australia. THE ROYAL SOCIETY OF NEW SOUTH WALES The Society originated in the year 1821 as the Philosophical Society of Australasia. Its main function is the promotion of Science through the following activities: Publication of results of scientific investigation through its Journal and Proceedings; the Library; awards of Prizes and Medals; liaison with other Scientific Societies; Monthly Meetings; and Summer Schools for Senior Secondary School Students. Special Meetings are held for the Pollock Memorial Lecture in Physics and Mathematics, the Liversidge Research Lecture in Chemistry, and the Clarke Memorial Lecture in Geology. Membership is open to any interested person whose application is acceptable to the Society. The application must be supported by two members of the Society, to one of whom the applicant must be personnally known. Membership categories are: Ordinary Members, Absentee Members and Associate Members. Annual Membership fee may be ascertained from the Society’s Office. Subscriptions to the Journal are welcomed. The current subscription rate may be ascertained from the Society’s Office. The Society welcomes manuscripts of research (and occasional review articles) in all branches of science, art, literature and philosophy, for publication in the Journal and Proceedings. Manuscripts will be accepted from both members and non-members, though those from the latter should be communicated through a member. A copy of the Guide to Authors is obtainable on request and manuscripts may be addressed to the Honorary Secretary (Editorial) at the above address. ISSN 0035-9173 © 1983 Royal Society of New South Wales. The appearance of the code at the top of the first page of an article in this journal indicates the copyright owner’s consent that copies of the articles may be made for personal or internal use, or for the personal or internal use of specific clients. This consent is given on the condition, however, that the copier pay the stated per-copy fee through the Copyright Clearance Center, Inc., 21 Congress Street, Salem, Massachusetts, 01970, USA for copying beyond that permitted by Section 107 or 108 of the US Copyright Law. This consent does not extend to other kinds of copying, such as copying for general distribution, for advertising or promotional purposes, for creating new collective works, or for resale. Papers published between 1930 and 1982 may be copied for a flat fee of $4.00 per article. JOURNAL AND PROCEEDINGS OF THE ROYAL SOCIETY OF NEW SOUTH WALES PARTS 1 and 2 VOLUME 116 (Nos. 327 and 328) 1983 ISSN 0035-9173 PUBLISHED BY THE SOCIETY PO BOX N112, GROSVENOR STREET, NSW 2000 iar A an aut } 7 + ee Bia Journal and Proceedings, Royal Society of New South Wales, Vol. 116, pp. 1-6, 1983 ISSN 0035-9173/83/010001 — 06 $4.00/ 1 Precise Observations of Minor Planets at Sydney Observatory During 1982 N. R. LOMB ABSTRACT. Positions of 1 Ceres, 3 Juno, 4 Vesta, 7 Iris, 39 Laetitia, 51 Nemausa and 704 Interamnia obtained with the 23 cm camera are given. The programme of precise observations of selected minor planets which was begun in 1955 has been continued and the results for 1982 are given here. This, however, is likely to be the last paper in the series. The methods of observation were des-— cribed in the first paper (Robertson 1958). All the plates were taken with the 23 cm camera (scale 116" to the millimetre). Two or four exposures were takeii on each plate, depending on the brightness of the planet. The number of exposures on each plate is indicated in Table 1. On some plates of the two brightest objects, 1 Ceres and 4 Vesta, an objective grating was used to give side images dispersed in right ascension; on these plates the side images of the minor planets were measured. In Table 1 are given the means of the posi- tions for all the exposures using all six reference stars at the mean of the exposure times. The result for the first pair of images was compared with that for the last two by adding the motion computed from the ephemeris for the plates with four exposures. The r.m.s. differences were 08009 Sec 6 in right ascension and 0714 in declination. No correction has been applied for aberration, light time or parallax, but the factors give the parallax correction when divided by the distance. The column headed "O-C" gives the differences be- tween the measured positions (corrected for paral- lax) and the position computed from the ephemerides Supplied by the Institute for Theoretical Astronomy in Leningrad. The ephemeris for 51 Nemausa was ob- tained from L.K. Kristensen (University of Aarhus, Denmark). In accordance with the recommendation of Commission 20 of the International Astronomical Union, Table 2 gives for each observation the positions of the reference stars and the six star dependences. The reference star positions were converted to standard coordinates for the calcu- lation of six star dependences. The columns headed "R.A." and "Dec." give the seconds of time and arc with the proper motion correction applied to bring the catalogue position to the epoch of the plate. The column headed "Star" gives the number of the star in the SAO catalogue or the zone and number of the star in the AGK3 catalogue. The column headed "Vol." gives the volume of the SAO or AGK3 in which the star is listed. The first column gives a serial number which cross- references Table 1 and Table 2 and also the catalogue from which the reference stars were taken. All plates were reduced by both the method of dependences and by first order plate constants using the same six reference stars. Equal results were obtained in each case, as could be expected due to the formal identity of the two methods. The r.m.s. residuals of the reference stars were obtained by taking for each star the mean residual from the plate constants fitted to the first and last pairs of images, summing the squares of these residuals in right ascension and declination for all stars on all plates with four exposures and dividing the result by the appropriate number of degrees of freedom. For SAO stars the r.m.s. residual was 0°69 (34 plates). Using six star dependences instead of two sets of three star dependences, as had been employed in reducing observations from years previous to 1978, has the disadvantage that a direct measure of the uncertainties in the measured positions is no longer available and the uncertainties have to be found by indirect means. The method used was des- cribed in a previous paper (Lomb 1980). The standard errors calculated in this way are listed in Table 3. As there were no four image plates with AGK3 reference stars the 038 r.m.s. residual for AGK3 stars in 1981 was used in calcu- lating the table. The plates were measured by Miss E. Burdis, Miss D. Teale and Miss R. Skeers. The observers at the telescope were D.S. King (K), N.R. Lomb (L), W.H. Robertson (R) and K.P. Sims (S). REFERENCES Robertson, W.H., 1958. Precise observations of minor planets at Sydney Observatory during 1955 and 1956. J. Roy. Soc. N.S.W. 92, 18-23 Sydney Observatory Papers No. 33. Lomb, N.R., 1980. Precise observations of minor planets at Sydney Observatory during 1979. od. Roy. Soc. N.S.W. 1138, 1-6 Sydney Observatory Papers No. 88. No. 1793 1794 1795 1796 17S 1798 199 1800 1801 1802 1803 1804 1805 1806 1807 1808 1809 1810 1811 1812 1813 1814 1S 15 1816 1817 1818 1819 1820 1821 1822 1823 1824 1825 1826 1827 1828 1829 1830 1831 1832 4 Vesta 1982 U.T. June 01.79287 June 22.73763 July 21.65403 July 29.63899 Aug. 09.59124 Aug. 19.55263 Aug. 23.54402 Sep. 07.48657 Sep. 24.45392 Oct. 13.41061 Oct. 18.40663 % ints: 1982 U.T. Feb. 03.73234 Mar. 22.57962 Mar. 29.55083 Apr. 22.49502 Apr. 29.45775 May 25.38542 June 17.34041 R. (1950.0) h m A. Ss 2187 . 140 426 - 107 - 336 -470 - (85 - 156 926 -058 109 - 339 -410 - 138 - 736 566 . 309 472 ~105 945 2025 shoo spec 340 ~ 344 586 564 -432 -324 = 10" -908 259 446 tes - 630 622 397 385 -907 .209 N. R. LOMB TABLE 1 POSITIONS OF MINOR PLANETS Dec. Parallax (1950.0) Factors fe) 1 " s " -09 42 20.05 -0.023 -3 -09 39 29.74 -0.004 -3 -09 15 24.18 +0.051 -3 -09 09 13.81 +0.012 -3 -09 O4 31.53 +0.036 -3 -09 02 11.37 +0.053 -3 -09 06 44.94 +0.013 -3 -10 00 14.87 +0.027 -3 -10 18 45.68 +0.034 -3 -10 48 26.53 -0.026 -3 -12 16 44.81 +0.032 -3 -13 16 41.53 -0.005 -3 -0O7 46 11.18 +0.036 -3 -06 47 51.38 -0.012 -3 -05 10 20.17 40.045 —-4 -O4 48 13.88 40.013 —-4 -05 33 01.83 -0.042 -4 -05 50 55.00 -0.007 —-4 -06 19 49.61 40.023 —-4 -07 32 48.48 -0.004 -3 -08 10 06.13 -0.018 -3 -08 32 00.56 +0.052 -3 -16 10 53.34 +0.011 -2 =—16 50 51.21 -0.006 -2 -19 52 02.82 -0.006 -2 -20 58 38.64 +0.029 -1 -22 28 07.53 -0.007 -1 -23 38 21.37 -0.023 -1 -24 01 44.20 -0.007 -1 -24 59 59.63 -0.039 -1 -25 10 26.31 +0.017 -1 -24 24 18.06 +0.032 -1 -24 03 58.09 +0.057 -1 -10 48 26.02 +0.014 -3 -08 32 02.43 +0.007 -3 -07 44 39.01 -0.009 -3 -05 08 12.70 +0.056 —4 -O4 32 44.18 +0.005 —-4 -03 23 32.00 -0.001 —-4 -03 43 06.56 +0.027 —-4 ane ee Jee ee ee a A NO) SPnorFrrererererere ete MPMMMNM FE EMNM PNP MMO FELL ADMWNADANANMrAT ANDTDWDANADAANATAN NNNDWNADWANAWNE ma~wwvrunowr No. 1833 1834 1835 1836 1837 1838 1839 1840 1841 1842 1843 1844 1845 1846 1847 1848 1849 1850 1851 1852 No. 1193 SAO 1794 SAO 1795 SAO 1796 SAO PRECISE OBSERVATIONS OF MINOR PLANETS TABLE 1 (Cont.) POSITIONS OF MINOR PLANETS RA Dec. Parallax (1950.0) (1950.0) Factors hm $s Oo rf ww s " 39 Laetitia 1982 U.T. May 24.76979 20 44 37.941 -08 14 31.57 -0.011 -3.79 -0 June 01.75393 20 47 18.080 -07 54 48.97 40.002 -3.84 -0 June 22.70415 20 47 17.205 -07 42 35.20 +0.026 -3.87 -0 July 21.59957 20° 31 20.317 -09 22 35.61 -0.019 -3.63 +0 July 28.58604 20 25 45.284 -10 05 30.22 40.010 -3.53 +0 Aug. 09.54798 20 16 13.994 -11 28 34.81 40.015 -3.34 +0 Aug. 19.50594 20 09 22.387 -12 41 04.39 -0.017 -3.16 +0 Aug. 23.50507 20 07 06.580 -13 09 41.72 40.020 -3.09 -0 Sep. 07.45035 20 02 '01...157 -14 47 58.66 -0.013 -2.86 +0 Sep. 24.42821 20503 312111 -16 13 49.43 +0.061 -2.66 -0 51 Nemausa 1962-U\T. Mar. 29.69034 15 03 13.898 -07 38 08.09 +0.002 -3.84 -0 Apr. 22.62065 14 49 53.035 -03 53 46.22 +0.018 —4.35 -0 May 17.54544 14 29 18.486 -00 48 33.25 +0.040 -4.75 -0 June 17.44298 14 18 09.626 -00 21 37.99 +0.009 -4.81 +0 June 22.,42947 14 18 44.403 -00 37 30.26 +90.008 -4.77 -0 June 28.43082 14 20 18.689 -01 02 23.32 +0.059 —-4.72 +0 704 Interamnia 1982 U.T. Jan. 21.67346 10 02 38.529 -05 41 05.48 +0.028 —-4.10 -0 Mar. 16.49644 09 22 05.111 -O4 21 20.47 +0.023 —-4.29 -0 Mar. 22.46031 09 19 17.692 =03 57 56.011 -0.031 —-4.34 -0 Mar. 29.47022 09 16 °55.273 -03 30 55.31 +0.063 —-4.40 -0 TABLE 2 REFERENCE STAR POSITIONS AND DEPENDENCES Vol. Star Depend. R.A. Dec. No. Vol. Star 3 140681 0.125936 48.831 26.12 1797 3 140453 3 140697 0.137305 18.282 54.86 SAO 3 140487 3 159467 O15 7554 165323 22,13 3 159224 3 140746 0.177822 50.825 26.42 3 159245 3 159515 0.197871 49.940 56.86 3 140537 3 140793 6.203512 31.628 C7237 5 140571 3 140681 0.219242 48.831 26.12 1798 3 140321 3 140713 0.216919 28.541 27.00 SAO 3 140361 3 159467 0.141128 16.323 22.13 3 159083 3 140778 OL 177581 23.343 58.34 3 140394 3 159515 0.109455 49.940 56.86 5 140412 3 140793 0.135674 31.628 Cia S 140432 3 140571 0.164689 36.888 50.28 1799 3 140294 3 140589 0.229048 24.977 26.55 SAO 3 140306 5] 140598 OF 107M 5i 25.658 Bese 3) 140307 3 140628 0.244369 08.361 25:0 | 140327 3 159383 0.074080 16.763 39.23 3 140341 3 140666 0.180657 33.491 40.96 3 140350 3 140518 0.144217 19.396 04.72 1800 5 158793 3 140530 0.159530 48.791 52.06 SAO 5 140135 3 140537 0.141363 17 «520 20.24 3 140162 3 159308 0.187767 06.612 27.68 3 158868 3 140587 0.172718 14.887 O1627 5 158886 3 140606 0.194404 03.045 02.20 5 140225 .008 SUIS -Us2 005 054 ste .026 2018 024 .006 ONS 004 Ou .018 .007 O42 053 052 041 087 qo0o0CO0CO C0O0O0 00 000000 000000000 Depend. «187707 .200078 - 146319 - 143762 PloeDDe «139582 - 182084 - 155698 - 185376 . 150093 ~174318 - 152430 . 195047 Actas - 196246 - 149290 «158557 - 127684 . 160047 - 155043 - 154093 2161123 - 179685 - 170009 No. Ex of p. Pm fee LF SEMN Po MM MM PY PNP MM PM PO ADNUDANNDUACA nAnarwmwunrn nwrn No. 1801 SAO 1802 SAO 1803 SAO 1804 SAO 1805 SAO 1806 SAO 1807 SAO 1808 SAO 1809 SAO 1810 SAO 1811 SAO Vol. WWW WW WD WWD WW WD WD WD WW WD WW WD WW W WW WW WWW WW WW WWW WWW WWW WW WW WW WW WW WW WW WW WW WW WW W WwW Star 158806 155810 140150 158844 140178 158854 158772 158793 158800 158834 158868 158886 158783 158800 158825 158868 158900 158902 158845 158872 158876 158910 158921 158936 142401 142440 1H2447 142496 142504 142535 142406 142436 142450 142486 142504 142524 142264 142272 142323 142366 142370 142388 142091 142116 142132 142142 142162 142187 141877 141887 141906 141909 141961 141989 141842 141868 141877 141906 141909 141924 141792 141808 141811 141868 141877 141887 oooo0co0ao0ao0cao0ao0coece0o0o0co0ceaoo0o0n0qoo0oo0o0o°0o0oo0o°0o0o°0oo°o 0 00 0e 0 0 0 00 0000 000 0 000000000 000 0 0000 C00 OO Depend. - 197164 - 190506 - 176299 » 150073 ~ 142821 2143137 ~212062 . 165697 2239427 . 105996 - 174488 rOZ3 sul - 193446 2 1953.14 sel" 159 - 125790 - 176473 - 131818 2135365 ~tt{2%e . 196717 - 140181 - 235861 - 174634 «219500 e235 0101 - 143947 - 184922 - 089533 . 130988 ~ 155941 - 189297 - 146332 - 196182 2171289 - 140959 - 189002 s25O13 - 140456 - 193996 2111579 ~ 149294 - 130416 192422 - 106336 - 238023 ~ 125109 -207094 - 196503 elTis3t ~ 102579 159356 «151020 - 133206 1235190 - 190980 - 202933 - 150625 . 109662 ~112045 - 174086 - 186340 «133752 - 149807 204704 «(5a 301 R. AS 292 7eeo 462 sets 353 «116 .020 433 O77 171 eei5 2855 2136 O77 -678 ep oot 1 -600 802 086 -266 .608 2234 .669 883 - 638 431 746 ae fe) Ot -990 743 .862 - 488 253) - 105 643 -310 -291 887 ~295 eeet 748 .208 046 ~985 171 ~154 aieon 964 ~495 724 897 -601 . 760 697 ofp ~495 724 Sood -910 2335 027 697 “ton 964 N. R. LOMB TABLE 2 (Cont.) REFERENCE STAR POSITIONS AND DEPENDENCES Dec. No. Sz SAO 1813 SAO 1814 SAO 1815 SAO 1816 SAO 1817 SAO 1818 SAO 1819 SAO 1820 SAO 1821 SAO 1822 SAO Vol. WWW WWW WW WW WW WWW WW WW WWW WW WWW WW WWW WW WW WW WWW WW WW WWW WW WWW WWW WW WW WWW WW WD Star 141725 141737 141792 141794 141835 141857 141707 141742 141756 141787 141811 141826 141725 141737 141763 141811 141818 141846 164517 164526 164585 164587 164624 164643 164635 164664 164673 164741 164774 164794 164567 190574 190622 164655 190683 164700 190487 190504 164567 190552 190594 190598 190322 190335 190391 190438 190472 190486 190190 190203 190248 190280 190322 190353 190110 190133 190190 190258 190271 190304 189957 189983 190006 190077 190104 190136 ooo0oo0oo0oo0oo0o°0oo0o°0co°0o°0co°0o0o0o0o0o cece 0ce 0e0e0 000 00000000 00C 0CCO0COCOCCOOCOCCOCOCOCOOCOCOCOCOCOCOCOCOCOCOCOCOCOCO8O 0 Oo Depend. - 171650 - 194747 - 183636 - 149001 - 145343 - 155623 - 11288: 214471 -093578 ~117894 . 267314 . 193862 . 186779 - 139:7 3% . 196744 - 140492 - 174319 - 161930 . 126780 - 141610 2 153003 - 181805 - 186166 ~ 209925 » ISDST - 142835 . 169767 . 161096 « 192272 Pes ao) «171539 . 184233 174175 «157683 - 157406 . 148764 - 189769 2177414 - 153055 » 175504 eas) - 146502 - 158484 - 204953 135547 . 205768 - 122902 - 172347, - 162482 si7 1230 - 159382 - 174993 . 163691 - 168221 167271 - 181008 - 148775 - 186208 2152231 - 164506 - 168683 - 146534 - 187904 - 144280 - 189214 - 163385 922 .818 . 706 No. 1823 SAO 1824 SAO 1825 SAO 1826 SAO 1827 SAO 1828 SAO 1829 SAO 1830 SAO 1831 SAO 1832 SAO 1833 SAO Vol. WWW WW W WWW WWW WWW WD WW WW WW WW WWW WWW WW WWW WW WWW WWW WW WWW WWW WWW WW WW WW WWW WW Ww PRECISE OBSERVATIONS OF MINOR PLANETS Star 189874 189894 189984 189991 190074 190077 189975 190018 190019 190136 190154 190203 190061 190074 190133 190135 190179 190203 157241 138772 Iai264 138810 1517336 Ibis 138456 138477 138487 138497 138515 138522 138394 138397 138434 138439 138450 138455 138235 138239 138262 138286 138301 138318 138198 138213 138218 138268 138276 138289 138213 138239 138244 138274 138276 138287 138334 138356 138361 138389 138400 138411 144746 144769 144780 144817 144851 144874 OOOO OOCOOCOOCOOCOCOO OOOO COOOOCOCOCOOCOOCOCOCMOCOCOCOCOCOaCoCoOCoCoCoCoCoaCoaCoaeoaCoaCoaoaCoaCoOOoaCoaMaCOCeCoaMaCoCaCOaCaCaCaCOaCOaCaCCO oO Depend. - 200343 . 158694 . 125463 ~203853 . 170746 . 140902 . 196113 . 178681 Shears}: siipd 122 ~ 144153 136432 «175166 184914 - 182059 - 150409 - 149346 . 158106 . 180673 abate . 189210 - 139672 Ailtelsisiays) - 148748 «210315 «tf2534 SST CSity - 144613 tao 122 2125628 - 152319 - 165386 - 182736 - 156848 . 162064 - 180648 ~210543 -211290 . 188065 «147434 + 136117 ~ 106551 - 162984 - 167867 - 160391 . 165457 . 172688 - 170614 - 194000 . 176329 - 173180 ~154911 - 153596 - 147984 . 161606 silster =c ll 905 site 705 -228169 - 168208 - 186342 - 166073 - 188923 - 140121 - 176911 - 141630 Rie A. -154 2514 . 182 586 Apis! .819 SSE! 642 «(32 . 706 ~057 2174 «329 Seats) Bee 2 it 3008 174 “8/2 2555 we - 389 eral fe! . 386 561 594 065 ~9D2 .129 aie) s153 v5D8 SSH Soo ~193 .098 - 348 743 927 .092 ae) «495 421 243 -981 .063 = Sh 469 242 Asi 246 961 all Sl 045 .659 669 S05 e202 S00) Heiee) 843 «493 -965 -450 -980 456 TABLE 2 (Cont.) REFERENCE STAR POSITIONS AND DEPENDENCES Dec. No. 1834 SAO 1835 SAO 1836 SAO 1837 SAO 1838 SAO 1839 SAO 1840 SAO 1841 SAO 1842 SAO 1843 SAO 1844 SAO Vol. WWWWW WWW WWW WD WW WW WWW WW WWW WWW WW WWW WWW WWW WW WW WWW WW WW WW WW WWW WW WW WWW WW W Star 144769 144806 144812 144899 144921 144934 144796 144807 144818 144851 144897 144916 144510 163658 144543 144600 163718 144643 163536 1635770 144438 144491 163647 163658 163396 163403 163438 163463 163498 163546 163298 163311 163314 163368 163395 163405 163262 163265 163303 163314 163361 163368 163185 163187 163232 1632511 163283 163303 163200 163216 163255 163278 163322 163364 140255 140277 140313 140327 140358 140365 140132 140154 140189 140197 140223 140226 OF OF Or O, Oro OOO OO CO. OO OO, OOOO OO OO) OOOO OOO © OO C' © Or OC. O,O7O) © @) oO OO OC O Co OC CO oO; OO Oo: @ © oo’ © Depend. - 194473 179184 s1e5ec6 slo ao 141293 - 141829 a OPO - 142094 .200661 ~ 114395 2122/1 + 163567 - 175550 . 200331 - 142288 Sa stecdsss| - 185302 «159276 161491 . 156354 Paiosiion . 178766 ~ 157879 270856 252446 - 163933 eeo1col .096976 095236 - 134208 ~205612 - 199216 - 189975 plooa2e9 lest o126251 - 192169 . 163804 - 200238 . 139247 . 136338 - 168204 - 170044 200253 - 101191 236888 ~ 118413 lysed) 234462 - 184565 «2 19568 . 129978 2155433 075999 - 143991 . 168657 - 147789 ~ 185644 179472 ~ 174447 082122 ot O9 | - 208433 - 141570 210208 "TOO oo 783 433 ee elati eel 2914 s201 - 687 6) -778 2328 .618 814 -071 246 «756 ~ 147 . 306 . 100 Sial - 788 ~ 309 eats No. Vol. 1845 8 AGK3 8 8 8 fs) 8 1846 8 AGK3 8 8 8 8 8 1847 8 AGK3 8 8 8 8 8 1848 8 AGK3 8 8 8 8 8 AGK3 SAO SAO Star Depend. - 0°1919 0.167256 = 1°1843 0.191854 = 0°1922 0.225710 - 191845 0.129153 - 091927 0.212598 - 191846 0.154029 - 0°1903 0.160508 - 0°1904 0.166480 #001737. 0.161121 = 1°1830 0.172659 = 0°1910. 0.173016 + 091743 0.166216 - 0°1905 0.167548 - 191827 0.194488 + 091734 0.130384 - 191832 0.205189 + 0°1741 0:142670 = 6°1911 0.159721 = 1°1827 0.228345 - 0°1906 0.208592 - 0°1909 0.169914 - 0°1916 0.099240 = 2° 864 ~06,.775923 - 191838 0.117986 TABLE 3 STANDARD ERRORS image image image Sydney Observatory, Sydney, N.S.W., 2000. R.A. 05012 sec 6 03020 sec 6 02020 sec 6 R.A. 39.483 44.729 37.120 28.202 12.063 33.887 30.306 13.945 04.780 10.158 36.354 02.060 15.881 04.175 53.234 14.333 00.228 59.049 04.175 02.138 32.555 32.134 04.155 Ulan a) (Manuscript received 23.2.83) N. R. LOMB TABLE 2 (Cont.) REFERENCE STAR POSITIONS AND DEPENDENCES No. 1849 SAO 1850 SAO 1851 SAO 1852 SAO Vol. WWW WW WW WW WWW WD WW WW WW WW WW WwW Star 137291 137308 13322 137356 137359 137368 136765 136783 136811 136834 136874 136891 136760 136765 136783 136798 136807 136834 136692 136729 136735 136765 136776 136796 ooooo0ooo0oo0o0o 00 0 0e 0 000 0000 0 Depend. 21367511 ~2 13630 086124 - 236907 Pulisiolsy ly/ - 190071 - 196694 - 136846 -216471 - 114940 - 209739 - 125344 3232819 - 203449 - 203362 » 132133 - 115746 - 112490 - 123406 « 170384 092578 - 239887 » 157305 2216444 202 645 353 - 398 915 .307 .534 -770 =901 . 180 944 915 . 307 450 462 TEGO 7035 . 806 .969 £915 435 3330 soe Journal and Proceedings, Royal Society of New South Wales, Vol. 116, pp. 7-10, 1983 ISSN 0035-9173/83/010007 — 04 $4.00/ 1 The Volatile Leaf Oils of Melaleuca armillaris, M. dissitiflora and M. trichostachya JOSEPH M. BROPHY AND ERICH V. LASSAK ABSTRACT. The composition of the steam-volatile leaf oils of Melaleuca armillaris, M. dtsstttf- flora and M. trichostachya has been determined by the use of capillary gas-liquid chromatography and mass spectrometry. whilst M. trtchostachya The oil of M. armillarts contained 1, 8-cineole as its main component leaf oil contained major proportions of both 1, 8-cineole and a-pinene. M. disstttflora was found to exist in two chemical forms characterized by oils rich in 1, 8- cineole and terpinen-4-o0l respectively. INTRODUCTION Following our earlier investigations of the volatile leaf oils of Melaleuca (Hellyer and Lassak, 1968; Lassak, 1979) we have now examined the oils of three species included by Bentham (1966) in the series Sptetflorae, Melaleuca armtllarts Sm., M. dtsstttflora F. Muell. and ™. trtchostachya Lindl. So far only the oil of ™. trichostachya has been examined. Baker and Smith (1910) reported 1,8-cineole as the main component (ca 80% of the oil) together with small amounts of terpinyl acetate and possibly of a-pinene in two samples of oil obtained from foliage collected near Gladstone in Queensland and Port Macquarie in northern coastal New South Wales. Since mM. trtchostachya does not appear to occur in its native state in eastern New South Wales, the Port Macquarie material was probably incorrectly ident- fred: It should be noted that all commercially produced Melaleuca oils derive from species belong- ing to Sptetflorae. M. caguputt Powell (as well as certain closely related broad-leaved Melaleucas growing in the Indonesian archipelago) and the cineole-rich form M. quinquenervta (Cav.) S.T. Blake (once incorrectly named M vtrtdiflora Gaertn.) yield the medicinal oils of 'cajeput' and "niaouli' respectively, whilst the fragrant nerolidol-rich form of the latter species has once been used for perfumery purposes. The terpinen-4-ol forms of M. alterntfolta Cheel and M. ltnaritfolia Am. yield oils with remarkable bactericidal properties (Penfold and Grant, 1926). RESULTS AND DISCUSSION Analysis of the freshly extracted steam- volatile oils by means of capillary gas-liquid chromatography (GLC) and mass spectrometry (MS) has shown that the oils of all three species are almost entirely monoterpenoid and qualitatively quite similar (Table 1). M. armillarts, a tall and densely leaved shrub of southeastern coastal Australia, commonly known as 'giant myrtle' yielded oils rich in 1,8- cineole (up to about 70%). Minor components included a-pinene, limonene and a-terpineol, whilst a-phellandrene was present in trace amounts only. M. dtsett2;lora, aishrub of ‘central Australia, yielded somewhat more variable oils. Those obtain- ed from foliage collected in the Davenport Ranges were invariably rich in 1,8-cineole and thus great- ly resembled the oil of M. armillarts, whilst oils extracted from trees growing near Charles River in the vicinity of Alice Springs contained terpinen- 4-ol as their main component with 1,8-cineole never exceeding 10%. It appears, therefore, that M. dissttiflora exists in two chemical forms character- ized by 1,8-cineole and terpinen-4-o0l respectively, a phenomenon previously encountered in the related species M. alterntfolia and M. ltnaritfolta (Penfold and Morrison, 1946; Penfold, Morrison and McKern, 1948; .Davenport, Jones and Sutherland, 1949) M. trtchostachya, a widely distributed Australian inland species, yielded a leaf oil rich in a-pinene and 1,8-cineole (52% and 30% respectively). Since only one sample of foliage was available for our study no conclusions can be drawn about the chemical variability of the oils of this species. The results reported by Baker and Smith (1910) on the oil from Gladstone suggest that compositional variation may be rather large. From an economic point of view M. armtllarts and particularly the terpinen-4-0l from of M. dtsstttflora may be promising. The comparatively high 1,8-cineole content of the leaf 01il of the former, its very low a-phellandrene content (undetectable by the usual nitrite phellandrene test) as well as its vigorous regrowth habit could make M. armitllarts an attractive alternative source of the medicinally useful 1,8-cineole. The consistently high terpinen-4-ol content of the Charles River population of M. dtssttiflora (Table 2) may allow its oil to be used in the same way as that of M. alternifolta for medicinal as well as flavouring applications. Being, unlike M. alter- ntfolta and M. linaritifolta, an inland species it may be suitable for the establishment of plantat- ions in the arid Australian outback. EXPERIMENTAL Collection of Plant Material and Isolation of Volatile Oils. Fresh foliage and terminal brachlets of M. JOSEPH M. BROPHY AND ERICH V. LASSAK TABLE 1. % Composition of Melaleuca Oils* Peak/ Compound M. armillaris M. dissitiflora M, trichostachya | Charles | Davenport Ranges — ——E—e Sa Smee te 1* 'o -thujene - OZ 2* x -pinene 1.4- 2.0 50.0 3 ' camphene ce ar er’, = = 4 . (3 -pinene 1.2- 1.6 0.4-14.7 , 0.7- 0.9 2.5 5 | sabinene 0.2- 0.6 | tr = 0.9%) tr. O46 0.3 6 ‘°(myrcene 2.1- 2.4 0.6- 1.3: 0O.5- 1.3 | dee 7 \& -phellandrene O.4= 0...2 6 coer eas tir. = 8 (i&-terpinene O.1- 0.3 508-10.1. tri= 1.574 O.1 9 , limonene 6.5= 7.9 | O.4- 1.5; 5.5- 6.7 Pa 10 | unknown = br 019) tr. - 14 ,1,8-cineole | 58.7-69.0 | 1.5- 7.3 '63.1-65.8 30%44 12 ,xX -terpinene | O.3- 0.8 }\12.0-18,2: 0.4- 5.8 0.5 13 | p-cymene | tr.- 0.5 1.7 -14,2 | O27 28 Ova 14 | terpinolene ©. 1— 0.23 | 2.0- 3.8: 3.1- 3.3 Orn2 15 ip, _~dimethylstyrene - tre. O22 ri On d= 0155 Oat 16 |unknown tri 0.4 | 0.10.67) tr. 0-6 - 47.) lanalooL tr c= 025 lotr .= 0.46) tr .— 0.2 - 18 |sesquiterpene Ci 5Ho4 - | 0.2 0.6 | - - 19 {sesquiterpene Ci sHog tres 1052 | O.7- 1.4 | tr.- 0.2 0.3 20 j|unknown | tr.= 0.2 l trie 0.2 | tr. 0.6 21 [unknown - - - 0.6 22 -~selinene ' tr.- 0.9 | = = 1.6 23 | cerpinen-4-ol | 0.7= 1,0 ~ 123 .1=52..8.|.1..5= 7626 1.4 24 |aromadendrene tr. Ons — IO 7 - = 25 | trans- PB -terpineol i tr.- 0.2 - tr.- 0.2 - 26 ; unknown tr = (O73 bre ON 2a tre Ol oe 0.2 27 jneryl acetate {enehes - tr.- 0.2 0.2 28 monoterpenoid alcohol O.2- 1.4 | O21 0.35)" O.2— 256 O22 | C10#18° | | 29 LGsgiyce tr O12 O.1- | 0.41=20..8 OS 30 poe geo neot 7,.5- 8.8 1.3- 2.7 | 4.4- 8.5 ileal Sal ‘X= terpinyl acetate | tr.- 0.5 are | tr = 0.4 tr 32 |sesquiterpene Ci cHog - : = | tr.=— 1,041 - 36) | seequiterpene Ci 5H 24 tr.=— 0.2 - - OF 5 34 | piper i tone : - tr.= 0.2 | tr.-— 0.5 - 35 j;geranyl acetate O75 — eo Rene Oe 0.3. css gar O72 36 | trans- piperitol - O..4=: 1,0. 4te.— 029 0.4 37°, ) 82 -p-cymenol 0.1 - tr. O72 - 38 | sesquiterpene Ci 5H 24 Osi=~ 150 = = = 39 |geraniol L 2054 = 085 EON1— O42) -tr.—1 0.5 Om 4O trans-nerolidol Ort = - O.1 41 |methyleugenol - - tr—) O39 Ome, 42 unknown - - - 1.3 43 ;unknown tr Oc - - 0.2 44 ‘unknown | 0.2 45 ‘unknown O33 46 ;unknown 0.2 *these two compounds co-injected on the FFAP ccated column but could be separated on a DC550 coated column. +tr.: (0.1% VOLATILE LEAF OILS TABLE 2. Qil Composition of Charles River Population of M. dissitiflora Sydney, N.S.W-. % M. dissitiflora Davenport | “12.98 Ranges, N.T. | to o 2515 | Charles River, 1.40 i N.T. to | 4,25 —— ———— 2 ie eR Dp Ce a et ea 5 seesttsatne pea M. trichostachya : Hugh River, 1.28 N.T. * Yield based on weight of air-dried plant Tree no. Terpinen-4-ol1 1,8-cineole content (%) content (%) 1 | 51.8 eel 2 46.3 5 3 38.6 aes) 4 39.5 LS 5 7 a7 foe 6 utopias E 135 7 251 Jiao TABLE 3. ' ! t . ; : i ; 20 20 Species Locality (Oe Yael: Ny Xp im V/W a A et = iad a ——— ae iq aatenchameurast can sremesenemner sop many am a M. armillaris Asquith and | 0.90 ‘1.4612 41.2 Berowra Hts. | to GO tO | north of 2 eto 14654 45.8 | { | M4658. 4004 ' to to : (1.4660 +2.0° (1.4630 +10.0° to ton. ‘4.4807 +414.8 y 1.4663 419.8" material, et tae mrp ae OZ 9095 to 0.9147 0.9144 to 0.9190 O7590¢6 to / 0.9144 0.8864 10 JOSEPH M. BROPHY AND ERICH V. LASSAK armillarts, obtained from cultivated trees growing at Berowra Heights and Asquith, and similar but air-dried material of M. disstttflora, collected at Elkedra and Bonney Well in the Davenport Ranges and at Charles River near Alice Springs, and of mM. trichostachya from Hugh River west of Alice Springs, were steam-distilled as described previously (Lassak, 1979) to yield colourless to pale yellow oils (Table 3). Botanical voucher specimens are lodged at the Biological and Chemical Research Institute (M. armtllarts) and at the Northern Territory Herbarium, Arid Zone Research Institute (mM. disstttflora and M. trtchostachya). Identification of 0il Components Analytical GLC was conducted on a Perkin Elmer Sigma 2B chromatograph using a 50m by 0.2mm i.d. FFAP coated fused silica column with He as carrier gas. Individual runs _ were temperature programmed from 80 to 170° at 6 /min following an initial holding period of 9 min at 80. Individual components were tentatively identified by their retention times and by co-injection with authentic compounds. A Perkin Elmer Sigma 10B Chromatography Data Station was used to determine percentage compositions. GLC/MS were determined using Shimadzu GC6-AMP gas chromatograph equipped with a FFAP coated SCOT column (105m by 0.5 mm i.d.) or an OV 17 coated SCOT column (109m by 0.5 mm i.d.) interfaced to an AEI MS-1w mass spectrometer through an all-glass straight split with He as carrier gas. The, gas chromatograph was programmed from 70 - 230 at 3° /min; the mass spectrometer operated at 70 eV with the ion source at 150 . Spectra were recorded and processed by a VG Digispec Display data system which produced standard bar graphs for direct comparison with published spectra. The following compounds were isolated by fractional distillation of the oils and their identities confirmed by their infrared spectra: a-pinene, 1,8-cineole and terpinen-4-01; the presence of piperitone was confirmed by its isolation (neutral sulphite method) followed by conversion to its 2,4-DNP derivative. Department of Organic Chemistry, University of New South Wales, P.O. Box 1, Kensington, NSW, 2033, Australia. (J.J. Brophy) ACKNOWLEDGEMENTS The authors thank Mr. R. Horner of Alice Springs for collecting samples of M. dtssitttflora and M. trtchostachya foliage, Mr. J. Maconochie, Northern Territory Herbarium, Arid Zone Research Institute, Alice Springs, for botanical identificat- ions, Mrs. J. Thompson, National Herbarium, Royal Botanic Gardens, Sydney, for helpful discussions and Miss A.F. Winterbotham and Mr. G.B. Speirs for technical assistance. REFERENCES Baker.,..R.T..and Smith, H.G:., 1900" On the Australian Melaleucas and their Essential Oils. Pawaeeer J.. &@ Proc. Roy. SoG iNGSsWe so. 592-615. Bentham, G., 1866. Flora Australienisis. Lovell Reeve & Co. London. Vol. 3, 123-126. Davenport, J.B., Jones, T.G.H. and Sutherland, M.D., 1949. Essential Oils of the Queensland Flora. XXIII. Re-examination of the Essential Oil of Melaleuca linarittfolta. Untv. Queensland Papers, 1, NO. <565,.1-125 Hellyer, R.O. and Lassak, E.V., 1968. The Steam- Volatile Constituents of Melaleuca viridtflora Sol. ‘ex Gaertn. , Aust. J. Chem. ,.21, 2585-2587. The Volatile Leaf Oils of J. @ Proce. hoy. Lassak, E.V., 1979. Three Species of Melaleuca. Soc. N.S.W., 112, 143-145. Penfold, A.R. and Grant, R., 1925. The Germicidal Values of Some Australian Essential Oils and Their Pure Constituents. Together with those for some Essential Oil Isolates and Synthetics. Part III. J. @ Proc. Roy: 50e. NasSwWesiods 346-350. Penfold, A.R. and Morrison, F.R., 1946. Australian Tea Trees of Economic Value. Sydney Technolog- ical Museum. Bulletin No. 14, Part 1, 3rd Ed. Penfold, A.R., Morrison, F.R. and McKern, H.H.G., 1948. Studies in the Physiological Forms of the Myrtaceae. Part II. The Occurrence of Physiological Forms in Melaleuca Alterntfolta Cheel. Researches on Essential Otls of the Australian Flora, 1, 18-19. Museum of Technology and Applied Science, Sydney. Biological and Chemical Research Institute, N.S.W. Department of Agriculture, P.M.B. 10, Rydalmere, NSW, 2116, Australia. (E.V. Lassak) (Manuscript received 23.2. 83) Journal and Proceedings, Royal Society of New South Wales, Vol. 116, pp. 11-15, 1983 ISSN 0035-9173/83/010011 — 05 $4.00/ 1 Lake Dieri and its Pleistocene Environment of Sedimentation, South Australia J. A. DULHUNTY ABSTRACT. Recent geological investigations have shown that the Oligocene Cordillo Surface (Wopfner, 1974) was deformed in mid Tertiary time into the Lake Eyre and Lake Frome structural basins separated by a positive tectonic divide. Thus, Lake Eyre and Lake Frome had separate late deposited on both sides of the divide. Sediments from late Tertiary to Holocene were Pleistocene ancestral lakes, and one large lake (Loffler and Sullivan, 1979) covering both structural basins, was unlikely to have occurred. It is proposed that the name Dieri should be preserved for the late Pleistocene ancestor of Lake Eyre, and the name Pilatapa could be used for the equivalent ancestor of Lake Frome. The occurrence of fresh and saltwater fossils in Lake Dieri sediments has been regarded as evidence of cyclic climatic variation. It is now suggested that salinity layering may have occurred due to fresh riverwater entering upper layers and overflowing to the sea, and highly saline groundwater entering through the lake bottom to form highly saline, heavy bottom water. INTRODUCTION Lake Eyre, to the northwest of the Flinders Range, and Lakes Frome, Callabonna, Blanche and Gregory, to the east and northeast (Fig. 1), are members of a family of contemporary ephemeral lakes in an arid environment. They developed during Holocene time from late Pleistocene ancestors which occupied the positions of the present lakes and extended beyond. The former lake which was the permanently-filled ancestor of present-day Lake Eyre, is known as Lake Dieri, the tribal name of Aborigines living in the vicinity. The history of the concept and naming of Lake Dieri has been reviewed by Loffler and Sullivan (1979). The idea of a lake in a more pluvial or wetter environment, overflowing to the ocean and eventually drying up with the onset of aridity to become present-day Lake Eyre, appears to have been first suggested by Gregory (1906) and then by Howchin (1909). Fenner (1931) and David (1932) later suggested that the ancestral lake could have embraced Lakes Frome, Callabonna, Blanche and Gregory. Browne (1945) first recorded the name Lake Dieri, acknowledging that it had been suggested earlier by Sir Edgeworth David (pers. comm.) but unrecorded, The name has since been used by other authors including King (1956), Johns (1963), Loffler and Sullivan (1979) and Dulhunty (1982). From the distribution of longitudinal sandridges and aligned transverse claypans, and interpretation of satellite imagery, Loffler and Sullivan (1979) suggested that Lake Dieri covered Lake Eyre, much of the southern Simpson Desert, the Tirari and Strzelecki Deserts and Lakes Frome, Callabonna, Blanche and Gregory. They also suggested that it might have existed over a long period of time extending back into the late Tertiary, and that it gradually diminished with many oscillations throughout Pleistocene time. They mapped the northern and eastern boundaries of aligned pans as limits of Lake Dieri in those directions, but did not show any boundaries west of Lakes Frome and Callabonna, or south and west of Lake Eyre. The purposes of this paper are (a) to support the general concept of late Pleistocene ancestral lakes, but to suggest that there were two main lacustrine areas of limited extent and duration rather than one large lake existing throughout Pleistocene time, (b) to show probable limits to the occurrence of late Pleistocene lakes west and southwest of Lakes Frome, Callabonna, Blanche and Gregory, and to the south and west of Lake Eyre, and (c) to suggest that salinity layering might have been an environmental factor in Lake Dieri contributing to simultaneous co-existence of fresh and saline conditions of sedimentation. EVOLUTION OF LAKE EYRE AND LAKE FROME DEPOSITIONAL REGIONS Results of recent investigations bearing directly on Cainozoic geological history of the Lake Eyre and Lake Frome internal drainage system, have been recorded by Callen (1977), Callen and Tedford (1976), Jessup and Norris (1971), Loffler and Sullivan (1979), Wopfner, Callen and Harris (1974) and Wopfner and Twidale (1967). From the foregoing recorded results, it is evident that the widespread deep subsidence, which formed the Great Artesian Basin and its Mesozoic sediments, came to a close in late Cretaceous and early Tertiary time with the deposition of 12 J. A. DULHUNTY LOCALITY N.TERRITORY Q’LAND S. AUSTRALIA 26° S LS ni (A. TERNAL -/ DRAINAGE “SYSTEM - GREGORY L. BLANCHE i ad NORTHEASTERN SOUTH AUSTRALIA SHOWING LAKE EYRE AND LAKE FROME STRUCTURAL BASINS LEGEND ——7” PROBABLE AREA OF LAKE EYRE BASIN \ WITHIN WHICH ANCESTRAL LAKE DIERI —— ~ OCCURRED eeecee**’ PROBABLE AREA OF LAKE FROME BASIN ., WITHIN WHICH ANCESTOR OF LAKE FROME 200°” ' OCCURRED GEESED contemporary EPHEMERAL LAKE BEDS / ip meciueae FEATURES P NTH. OLARY procs (AFTER WOPFNER & TWIDALE, 1967, CALLEN, 1977) \ Cees Ce ee 9 008? PP00e4 *e je y eoccce ° = bay fea) Fag. 1. Areas of structural basins within which late Pleistocene ancestors of Lake Eyre and Lake Frome could have occurred. LAKE DIERI ENVIRONMENT OF SEDIMENTATION 13 Palaeocene -— Eocene Eyre Formation in central and southwestern areas of the basin. As it waned subsidence contracted to the southwest giving the basin and its sediments a very gentle tilt in that direction. This, together with mid Tertiary movements, provided the basic setting for subsequent Pleistocene development of the present-day Lake Eyre internal drainage system with its Lake Frome sub-basin, The deposition of the Eyre Formation was followed by a long non-depositional period in Oligocene time during which the Cordillo Surface (Wopfner, 1974) formed with its encrustation of early Tertiary silcrete. During late Oligocene or early Miocene time the surface was deformed in the southwestern Great Artesian Basin, and subdivided into two large structural depressions which became separate depositional regions after mid to late Miocene time. One of these covered Lake Eyre, the southern Simpson Desert and Tirari Desert, and the other covered the Lake Frome and Strzelecki Desert region including Lakes Callabonna, Blanche and gregory. They are referred to as the Lake Eyre Basin and Lake Frome Basin. The two were separated by a zone of positive tectonic features running generally north from the Flinders Range along the Dulkaninna and Mt. Gason Uplifts to the Vicinity of Birdsville (Figs 1 & 2). The Birdsville Track now follows the more elevated and less sandy country along the positive tectonic zone, From about mid or late Miocene to early Pliocene the two depressions became depositional. The Namba Formation was deposited in the Lake Frome Basin and the Etadunna Formation in the Lake Eyre Basin. Then, following another non-depositional interval in Pliocene time, the late Pliocene - early Pleistocene Millyera Formation accumulated in the Lake Frome Basin. Equivalent early Pleistocene sediments have not yet been fully investigated in the Lake Eyre Basin, but they are almost certainly present to a greater or less extent (Stirton, Tedford and Miller, 1961). Another non-depositional period would seem to have occurrred about mid Pleistocene time during which the Flinders Range continued to rise (Callen, 1977) and post Etadunna movement occurred along the tectonic divide between the two basins in each of which further depression occurred. Then, as a result of a wetter climatic phase (Bowler, 1978) in late Pleistocene time, more or less permanently filled lakes developed on both sides of the tectonic divide, which would appear to have risen to no more than 40 m above the beds of the two lakes in some places, but over 200 m at others. They were separate lakes but if filled to over about 40 m deep, then water could have flowed between them through a relatively narrow channel between the south end of the Mt. Gason Uplift and the north end of the Dulkaninna Uplift, where Cooper Creek now flows from the Strzelecki Desert to the Tirari Desert (Fig. 1). In the late Pleistocene lake of the Lake Frome Basin the Eurinilla Formation was deposited disconformably upon earlier Pleistocene sediments. In the Lake Eyre Basin a widespread lake developed in which late Pleistocene sediments accumulated disconformably upon early Pleistocene beds in some places, and unconformably on Tertiary, Mesozoic and metamorphic basement rocks beyond the areas of early Pleistocene sediments (King, 1955; Wopfner and Twidale; 1967% Callen and Tedford, 1976). Deposition then ceased in both basins as they dried up with the onset of aridity towards the close of Pleistocene time. After some deflation during intense aridity, further depression and gentle folding in the Lake Eyre Basin and a return to a less arid phase with arise in watertable (Dulhunty, 1982), Holocene sedimentation commenced on both sides of the dividing ridge (Fig. 2). The Coonarbine Formation was deposited in Lake Frome, and equivalent sediments, as yet unnamed, commenced depositon in Lake Eyre (Dulhunty, 1982). LAKE DIERI, ANCESTOR OF LAKE EYRE In view of the foregoing relations between tectonic and depositional histories in the Lake Eyre and Lake Frome Basins, the following suggestions are offered: ilies The idea of Lake Dieri being one large lake covering both basins throughout part or all of Pleistocene time, must now be modified to a concept of early and late Pleistocene lakes separated in time by a mid Pleistocene non-depositional interval, and occurring in each of two basins separated geographically by a structural high. Qe With respect to the work of early Australian geologists, the name Lake Dieri should be preserved and used as the name of the late Pleistocene ancestral lake in the Lake Eyre Basin, from which present-day Lake Eyre descended. If a name is required for the late Pleistocene lake in the Lake Frome Basin, which was the ancestor of Lake Frome and in which the Coonarbine Formation was deposited, then the tribal name Pilatapa of Aboriginal people previously living in the vicinity of Lakes Frome and Callabonna, could well be used (Dr. L. A. Hercus, pers. comm.; Tindale, 1974). LATE PLEISTOCENE ENVIRONMENT OF SEDIMENTATION IN LAKE DIERI Lake Dieri received drainage from a catchment area very Similar to that of the present-day Lake Eyre internal drainage system. It occupied the present position of Lake Eyre, and it is believed by the author and others including Gregory (19045), Johns (1963) and Callen (1977) to have had an outlet to the sea. In addition to riverwater, Lake Dieri received large volumes of groundwater as its bed would have been the sump, or focal area, for movement of groundwater in the whole of the drainage system. Owing to low surface level, poor drainage and cyclic aridity in the central Great Artesian Basin area in Tertiary and early Pleistocene times, and the great thickness of underlying Cretaceous marine sediments that had never been appreciably elevated above sealevel, the groundwater must have been very saline around Lake Dieri. Thus its inflow must have been an important factor influencing salinity of the lakewater. 14 J. A. DULHUNTY TECTONIC DIVIDE LAKE EYRE BASIN LAKE EYRE LAKE FROME BASIN : PLEISTOCENE SEDIMENTS ETADUNNA-—NAMBA FORMATIONS LATE TERTIARY Papo 2% Sediments deposited in the southwestern area of Lake Dieri now outcrop in cliffs and steep shoreline slopes along the southern shores of Lake Eyre North, between Willow Head and Price peninsula (King, 1956; Johns, 1963). Outcrops up to 13 m thick were measured by the author along the southern shores of Madigan Gulf, and at Shelly Island. At least 4 m appeared to have been removed by weathering and erosion, making a probably minimum original thickness of some 17 m. King (1956) described a section of almost 10 m in the same vicinity. Lake Dieri sediments have yielded both freshwater and brackish to saltwater fossils, including Coxiella gilesi, foraminifera, fish bones, Diprotodon and crocodile remains (Stirton et al., 1961; Wopfner and Twidale, 1967), Chara and ostracods (King, 1956; ohms — 1963). Consequently the environment of the lake has been regarded variously in the past as either fresh, brackish to salt, or as alternating within such limits with cyclic variations in climatic phases. After recent field observations, consideration of environmental factors and stratigraphical relations, as well as the probability of a wetter climate with lower evaporation and higher watertable levels in late Pleistocene time (Bowler, 1978; Dulhunty, 1982), it is now suggested that Lake Dieri might have been a permanently-filled lake during a time interval of the order of 20,000 to 45,000 years b.p. Also that freshwater and saline environments of sedimentation might have co-existed as a consequence of salinity layering. This could have developed by continuous addition of fresh riverwater from the north and northeast to upper layers of lakewater and their escape to the south into the sea, concurrently with subterranean inflow of saline groundwater, through the lake bottom, into lower layers of bottom water. Such circumstances could have supported freshwater Section A-B across Fig. 1, showing relations EYRE FORMATION — EARLY TERTIARY WINTON FORMATION — CRETACEOUS Wa Oy) METAMORPHIC BASEMENT between structural development and stratigraphy. organisms and condition in light upper layers and along shorelines, and also, at the same time, saltwater organisms and conditions including deposition of gypsum in heavy bottom layers. As a consequence, simultaneous deposition of fresh and saline sediments could have occurred. Also a inixed-facies sediment could have formed where freshwater debris sank and became entombed in the saline environment. An example of salinity layering and co-existence of relatively fresh and highly saline environments developed in Lake Eyre during the 1974 filling (Dulhunty, 1977: 1982). If the temporary wetter climate that occurred in the Lake Eyre region during almost 7 years of the filling had prevailed as it did in Lake Dieri time, inflow of riverwater would have continued, and shoreline and upper water would have become virtually fresh, and continued to co-exist with the saline bottom water. However, though the 1974 filling was only transient, it could be regarded as a very short-lived reversion, possibly approximating to the late Pleistocene climate of the Lake Dieri environment, The possible development of salinity layering in Lake Dieri, by subterranean inflow of highly saline groundwater into bottom waters, would appear to be very similar to hydrological processes operating in present-day lakes in different parts of tne world (D. K. Hobday, pers. comm.; FEugster and Hardie, 1978; Hardie, 1968; Hardie, Smoot and Eugster, 1978). ACKNOWLEDGEMENTS It is wished to ackcnowledge valuable discussion with Dr. D. K. Hobday of Bridge Oil, Sydney, Dr. J. M. Bowler of Australian National University,.and Dr. R. J. Wasson of CoS usr OF, Canberra, the assistance of Muloorina Station in field activities at Lake Eyre, and research LAKE DIERI ENVIRONMENT OF SEDIMENTATION IS) facilities provided by the Department of Geology and Geophysics, University of Sydney. REFERENCES Bowler, J. M., 1978. Glacial age aeolian events in high and low latitudes: A Southern Hemisphere perspective, in ANTARCTIC GLACTAL HISTORY AND WORLD PALAEOENVIRONMENTS, np. 149-172. E. M. Van Zinderen Bakker (Ed.). Balkema, Rotterdam. Browne, W. R., 1945. An attempted post Tertiary chronology for Australia. Presidential Address. Proc. Linn, Soc. N.S.W., 70, 5-25. Gallen. Re As. 197!. Late Cainozoic environments of part of northeastern South Australia. Om geols Soe. Aust., 24(3), 161-170. Callen, R. A. and Telford, R. H., 1976. New late Cainozoic rock units and depositional environments, Lake Frome area, South Australia. limans ti SOC LOs AUSE sy 100IC3)i, 113-116. David, T. W. E., 1932. Explanatory notes to accompany a new geological map of the Commonwealth. Ist edn. Arnold, London. Dulhunty, J. A., 1977. fillings of Lake Eyre. Aust... 101(6)-, 147=15 1. Salt crust solution during Pranisis (Ke, SOCe to7 Duthunty., Je As, 19825 Holocene sedimentary environments in Lake Eyre, South Australia. J. geol. Soc. Aust., 29(4), 437-442. Eugster, Wi. Ps. and Hardie, L. A., 1978. Saline lakes, in PHYSICS AND CHEMISTRY OF LAKES. A. Lerman (Ed). Springer-Verlag, New York. reemmen., Ge. 193. geographical study. Tombs, Melbourne. South Australia: a 1st edn. Whitcombe and Fenner, ©C., 1952. muds, salts, etc. HOC), 235=258:. Lake Eyre in flood, 1950 - Trans. R. Soc. S. Aust., Gregory, J. Ws, 1906. The dead heart of Australia. 1st edn. Murray, London. Hardie, L. A., 1968. The origin of Recent non=-marine evaporite deposits of Saline Valley, Inyo County, California. Geochim. Cosmochim. Acta, 825 27913011. Department of Geology and Geophysics, University of Sydney, N.S.W., 2006, Australia. (Manuscript Hardie, L. A., Smoot, J. P. and Eugster, H. P., 19738. Saline lakes and their deposits: a sedimentological approach, in MODERN AND ANCIENT LAKE SEDIMENTS. A. Matter and M. E. tucker CEdS.)y. Spec. Publis.) dnt aeisse sediment., 2, 7-41. 1909. The geography of South lst edn. Whitcombe and Tombs, llowchin, W., Australia. Auckland. Jessup, R. W., and Norris, R.M., 1971. Cainozoic stratigraphay of the Lake Eyre basin and part of the arid region lying to the south Je geol, soc. Aust., 1603), 303-331. Johns, Re K., 1963: Investigation of Lake Fyre. Pit. alle og REPORT OF INVESTIGATIONS NO. 24, pp. 1-41. Dept. Mines, S. Aust. King, D., 1956. The Quaternary stratigraphic record at Lake Eyre North and the evolution of existing topographic forms. Trans. =R Soc. So. Aust., 19, 99=103. Loffier:. E. and Sulvivan, MM. E., 1979: Lake Dieri resurrected: an interpretation using satellite imagery. Z. Geomorph.. N.E., 2303), 233-242. Stintony Ra Aue tedrorda Ry He -and: Miller, Ae. 1961. Cenozoic stratigraphy and vertebrate palaeontology of the Tirari Desert, S. Aust. Rec. S. Aust. Musueun, 14(1), 19-61. Springs Re iGey, W900. The Great Artesian Basin in South Australia. Js Geol, Hoc. Aust.:,.5, 88-101. Tindale, Ne D., 1974. Aboriginal “tribes (on Australia. 1st edn. University of California Press, San Francisco. Wopfiner, H.,- 19/2. Depositional history and tectonics of South Australian sedimentary basins, Min. Res. Rev., S. Aust., 13 3); 32-50. Vopfner, H., 1974. Post Eocene history and stratigrapahy of northeastern South Australia. Transe lie SOC. oO. AUSts, 90, lle). Woptner, i.) aud Twidale, C2 Ra, 1967. Geomorphological history of the Lake Eyre Basin, in LANDFORM STUDIES FROM AUSTRALIA AND NEW GUINEA, J. N. Jennings and J. A. Mabbutt (Eds). A.N.U. Press, Canberra. Wopfner, H., Callen, R. and Harris, W. K., 1974. The lower Tertiary Eyre Formation of the southwestern Great Artesian Basin. J. geol. SoCs AUS UA. cio Itoi received 1.3.83) Journal and Proceedings, Royal Society of New South Wales, Vol. 116, pp. 17-23, 1983 ISSN 0035-9173/83/010017 — 07 $4.00/ 1 Silcretes in the Cobar Area, New South Wales R. A. GLEN AND J. T. HUTTON ABSTRACT. A recent, detailed geological survey of the Cobar area in central-western New South Wales has disclosed areas of silcrete development. In hand specimen and in chemical analyses, these silcretes closely resemble previously known occurrences found west of Cobar (Dolo tlills, N.S.W.) and northwest of Cobar (Tibooburra area, N.S.W. and adjacent area in southwest Queensland). however, on outcrop scale Cobar silcretes differ from those further west in that they form only localized occurrences, rather than extensive sheets. Localities, descriptions in hand specimen and thin section, and chemical analyses are given to document these silcrete occurrences. Although Wasson et al. (1979) have rightly questioned the earlier report by Dury (1966) of silcrete occurr- ences around Cobar, the new data presented here enable the Cobar area to be retained as a sitcrete, locality. INTRODUCTION The map of Stephens (1971) showing the distribution of silcretes in Australia would Suggest that silcretes should be found in the Cobar area of New South Wales (Fig.l, inset). Dury (1966) reported finding what he described as silcretes in this area, but Wasson et al.(1979) have rightly indicated that the materials described by Dury are not silcrete in the generally accepted definition. In their concluding comments, Wasson et al. (oy Oe pel soestated War. at 1s necessary to question the validity of any aspect of the geomorphic history of the Cobar area dependent upon the recognition of silcrete ...". Lest this Sentence be construed to imply that silcrete does not occur in the Cobar aréa, this present note documents several such occurrences, TERMINOLOGY There is no hard and fast definition of Silcrete. There is a general consensus of Opinion in the papers in "Silcrete in Australia" (Langford-Smith, 1978), that silcrete is a hard, indurated rock, composed mainly of quartz grains, occasionally with quartz "eyes", and cemented by fine-grained silica. Silcrete has a concho- idal fracture, due to equal hardness of frame- work grains and cement. Foreign minerals are either very rare and/or extremely small. Commonly associated with these easily recognized silcretes may be rocks showing secondary silica enrichment. These rocks are softer and break more irregularly than silcrete. They may also contain more evidence of the precursor rock-type. SILCRETES IN THE COBAR AREA Hand Specimen Description Silcretes in the Cobar area vary in colour from white through yellow to red, and there is some development of iron-stained rinds. True Silcretes are hard and break smoothly with a conchoidal fracture. Quartz "eyes" are present in some cases. Intermixed on outcrop scale with these easily recognized silcretes are white to red coloured rocks showing secondary silicific- ation. These break irregularly, reflecting irregular hardening, and may display linear, rod- shaped structures similar to those of Wopfner (1978; Fie. 10). Quartz “clasts may be present in these rocks as well as in the true silcretes. Baker (1978) noted that silcrete may be commonly associated with ferricrete. Distribution and Nature of Occurrences Silcrete bodies found in the Cobar area during the course of a regional mapping programme by the Geological Survey of New South Wales are shown in tigure 1. Most of the silcrétes occur in areas underlain by sediments of the Early Devonian Cobar Supergroup, with only limited development on areas underlain by basement rocks. These two units generally form subdued to poor outcrop and silcretes occur at a range of topo- graphic heights, not necessarily on high hills or peaks (Fig.1). In areas of the Cobar Supergroup high points are generally underlain by sandstone- rich lithologies,only some of which are silicified. In these cases,silcrete forms a capping and may also extend patchily down the hill slope. On other high points,alteration is restricted to the formation of minor weathering skins (compare data on the Biddabirra Hill site - BH Fig. 1 - between Dury 1966 and Wasson et al. 1979). The absence of silcrete from rocks of the Mulga Downs Group overlying the Cobar Supergroup is surprising. Despite the large amount of sandstone in the sequence, which has localized the formation of cuestas occupying some of the highest country around Cobar, (near) surface alteration is restricted to the formation of weathering skins, caused by the removal of iron oxides from the rock (compare data on the 18 Fig. 1 R. A. GLEN AND J. T. HUTTON REFERENCE Silcrete Occurrences Rene SOTO Mt. Hope Inset - Australia showing location of Cobar (C), Dolo Hills (D) and Tibooburra(T). L/S line from Stephens (1971). - silcrete inside the line, laterite outside the line. Main Figure - Simplified geology of the Cobar area, modified from Baker (1977), Felton (in press),Glen et al, (in press), Sizes of silcrete bodies have been exaggerated. Approximate topo- graphic heights of silcrete bodies from base geological maps: A-1 200m, A-2 200°m, Ba-1 200*m, Bb< 200m, Ba (NW) ~ 200m, Bb-1 220m, C-1 < 200m, C ?20Qm (mid north), 200 m (northwest), Da 220m, Db 260m, E < 240m, F ~ 200 m, G 200m, H 240 m, I 220 m, BH (Biddabirra Hill) peak 270m, BM (Mt Buckambool Peak) 405m. SILCRETES IN THE COBAR AREA 19 Mt Buckambool site - MB Fig. 1 - between Dury 1966 and Wasson et al. 1979). The silcretes we have seen in the Cobar area do not form extensive sheets such as those described from S.A. by Wopfner (1978) and from the NW corner of NSW by Watts (1978). Rather, individual outcrops are generally small (tens to a hundred square metres in area) and most of the silcrete occurrences in figure 1 consist of individual boulders and pebbles separated by, and lying in, recent fine-grained eluvium. At locality A-1 (see below), outcrop is more continuous and silcrete forms relics of a thin crust on granite. Around the northwestern part of the Louth Rd in fig.1, silcrete boulders, generally covered by eluvium, probably form part of a partly buried surface. It would thus appear, that what we see at Cobar may be relics of more extensive silcrete deposits, that have either been partly buried and/or partly broken up and removed. The absence of a widespread sheet probably accounts for the non recognition of silcrete in the past. Silcrete Associations As outlined above, silcrete generally occurs as variably-sized fragments in eluvium. however, from relations in some areas, it is possible to categorize silcrete occurrences into four types, based on their lithological relationship. A. Silcrete on basement granite Baker (1977, 1978) first noted and mapped occurrences of silcrete on the basement Tinderra Granite in the northeast part of the area in figure 1. Relations are probably best preserved at locality A-1 (Fig.1) where blocks of silcrete up to 0.3 m thick lie on poorly exposed weathered granite. Silcretes around locality A-2 probably also lie on granite subcrop. However, they also lie near sediments and the underlying lithology is not known with certainty. Pad Be Silcrete on the Cobar Supergroup Two lines of evidence suggest that many Silicretes: 11 the. northem part of the area are localized on sandstone-rich zones within the Cobar Supergroup. The first line of evidence consists of Silcrete on hill summits where it overlies marker sandstone-rich zones of the Cobar Supergroup which outcrop further down the hill slope (Ba, Ba-1 Fig.1). Silcrete here varies from boulders and pebbles in eluvium to iron-stained, fractured sheets of small outcrop (tens of square metres) up to lm or so thick. In the second line of evidence, silcrete outcrop in slightly elevated areas lies along strike from sandstone zones in the Cobar Supergroup. Silcrete here generally consists of loose material, or as small fractured outcrops (Bb, ?Bb-1,Fig.1). C. Silcrete on Cainozoic Conglomerate The presence of Cainozoic conglomerates in the Cobar district (mainly south and east of, or towards the south of, Fig.l) has been recorded in mapping by the New South Wales Geological Survey. The presence of similar conglomerates in the north- western part of the area in figure 1 is suggested by the local existence of a thin veneer of rounded pebbles of vein quartz and iron-stained sandstone freed by erosion, and by blocks of conglomerate containing clasts of vein quartz and sandstone in an iron-rich matrix. Most of these conglomerates show secondary silicification and some may be classifieds as truce silcretes. (C, \Fae.])> D. Silcrete on Pallid Zones In two areas - locality Da at a breakaway near Tinderra Tank (Baker 1977) and locality Db at a quarry near Rookery Homestead (Brown 1976) - Silcretes are underlain by a pallid zone. Relations are best described from the second site (Fig.2). Here rubbly silcrete at the surface passes down through 2 m.of crudely fractured ,silicitied rock into a pallid zone which consists of quartz and kaolinite with minor illite and smectite (2. olansky, pers. comm. ).. @inese relations are Similar to those described by Wopfner (1978), although in neither of the localities is the material below the pallid zone exposed. Thin Section Descriptions Silcrete samples were collected for petro- graphic examination from several of the localities shown in figure 1, Typical ones are described here. Silcrete developed from granite at locality A-1 shows typical "terrazzo" textures of Smale (1973), with irregular shaped quartz grains in a uniform dark matrix. (Fig. 3a). Silcrete over- lying sandstone at locality Ba-1l is similar (Fig.3b). It shows embayed and half-rounded to angular quartz grains in a cloudy-brown matrix containing a mass of fine shards. Of interest is the presence of accessory zircon and tourmaline inherited from the host rock. A thin section of silcrete from locality C-1 (possible developed on Cainozoic conglomerate) shows quartz grains less irregular and more round than described above (Fig.3c). Nor is the matrix as uniform, consisting in different areas of opaque material and very fine-grained quartz crystals. Chemical Analyses (Table 1) Chemical analyses of four silcretes from the Cobar area were carried out by X-ray fluorescence spectrometry (method of Hutton and Elliott, 1980). Table 1 shows that these Cobar silcretes are Similar to silcretes from the Dolo Hills, about 220 km to the west, reported by Hutton et al. (1978), and from Tibooburra silcretes, about 420 km to the northwest, reported by Hutton et al. (1978). They are also similar to the average composition of 63 silcretes reported by Watts (1977) from northwestem New South Wales and southwestern Queensland. Cobar silcretes have the usual low values of most elements except those associated with minerals that are resistant to weathering e.g. silicon, titanium and zirconium. The average of 0.95% Ti and 0.033% Zr for the four Cobar samples (Table 1) are both twice that of the average crustal abundance, namely 0.44% Ti and 0.016% Zr (Mason 1966). 20 R. A. GLEN AND J. T. HUTTON Silcrete occurrence at locality Db, exposed in quarry face. Rubble silcrete at surface overlies crudely columnar silcrete and silicified rock which passes down into pallid zone of quartz + clay minerals. Columnar silcrete about 2m thick. Thin Section photograph of silcretes. Good "terrazzo" texture from locality A-1. Angular to semi-rounded and embayed quartz grains in an opaque matrix. Cross nicols. Bar scale 5 mm. SILCRETES IN THE COBAR AREA 21 Fig. 3b Thin Section photograph of silcretes. Good "terrazzo" texture from locality Ba-1. Corroded and embayed quartz grains in an opaque matrix. Cross nicols. Bar scale 0.25 mm. Fig. 3c Thin Section photograph of silcretes. Silcrete from locality C-1, see text for description. Cross nicols. Bar scale 5mn. 22 R. A. GLEN AND J. T. HUTTON Analyses of Cobar silcretes and comparison with other silcretes in far western N.S.W. and southwestern QLD OTHER SILCRETES 1 Dolo Hills Tibooburra Tibooburra Av. of 63 from 5291 531Al — SW QLD and NW N.S.W. 2 O.14 0.03 0.09 0.04 OZ 0.11 0.23 0.24 47 46 46 45.2 0.1 0.02 0.02 2 0.03 0.01 0.01 0.03 0.21 0.02 0.04 0.06 1.4 0.7 0.9 0.88 0.5 0.7 0.6 ale 0.055 0.015 0.069 z 25 47 13 1. from Hutton et al (1978) Table 1: COBAR SILCRETES Locality A-1 A-2 Bb-1 C-1 Element Mg, % 0.01 0,01 O07 0.01 Al, % 0.28 0.18 0.12 0.06 Si % 46 AS 46 46 Poo 3% 0.01 0201 O0L 0.01 K, % G02 0.03 0.06 0.03 Ca, % 0.02 0.02 0.02 0.02 Ta, On7 1 | 0.6 134 Fe total,% 0.02 0.07 0.1 0.1 Zr, % 0.022 0.031 0.018 0.059 iby Eg 52 35 53 24 2. from Watts (1977) CONCLUSIONS Although Wasson et al. (1979) pointed out that Dury's (1966) ''silcretes'' would not be called such today, their own paper should not be taken to deny the presence of true silcretes in the Cobar area. The samples described above are lithologically (both in hand specimen and in thin section) and chemically similar to silcretes described from further west and northwest in New South Wales and adjacent areas in Queensland. Cobar silcrete is characterized by the dominance of silica minerals. Titanium minerals are also present, as indicated by chemical analyses and are generally fine-grained. Minerals contain- ing aluminium are absent. In the literature, Silcretes are associated with highly weathered profiles, with highly weathered sediments, such as the early Tertiary Eyre Formation, with quartz rich sandstones, and with granite (Wopfner 1978, Senior 1978). Similar associations occur at Cobar, with the addition of silcrete developed on Cainozoic gravels. Table 1 shows a marked chemical similarity of silcrete developed from different rock types. However, the different size ranges of quartz clasts in different silcretes help to differentiate those formed from fine- grained sandstone from those formed from coarser- grained conglomerate or granite. In/near situ development of silcrete is therefore suggested. Formation of the Cobar silcretes at different topographic heights (Fig.1) is not consistent with Dury's (1966) concept of a single pediplained surface, ACKNOWLEDGEMENTS Chemical analyses of silcrete samples were made by J.T.H. while an officer of the C.S.1.R.O. Division of Soils, Adelaide. The help of C.B. Wells of the same Division in the taking of the photomicrographs Figs. 3a and 3c is gratefully acknowledged. C.J. Baker is thanked for reading a draft of the paper. R.A.G. publishes with the permission, Secretary, NSW Department of Mineral Resources. REFERENCES Baker, C.J., 1977. Cobar 1:100,000 Geological Sheet 8035. New South Wales Geological Survey, Sydney. Baker, C.J., 1978. Geology of the Cobar 1:100,000 Sheet 8035. New South Wales Geological Survey, Sydney. Brown, R.E., 1976. Stratigraphic and structural interpretations of the Cobar Group and older units between Nymagee and I1lewong, central New South Wales. New South Wales Geological Survey - Report GS 1976/425 (Unpubl.). Dury, G.H., 1966. Duricrusted residuals on the Barrier and Cobar pediplains of New South Wales. od. Geol. Soc. Aust., 13, 299-307. SILCRETES IN THE COBAR AREA 3: Felton, E.A. in press. Canbelego 1:100,000 Geological Sheet 8134. New South Wales Geological Survey, Sydney. Glen, R.A. Felton, E.A. and Brown, R.E. in press. Wrightville 1:100,000 Geological Sheet 8034. New South Wales Geological Survey, Sydney. Hutton, J.f. and Elliott, S.M., 1980... An accurate XRF method for the analysis of geochemical exploration samples for major and trace elements using one glass disc. Chem. Geol., 29, 1-11. Hutton, J.T. Twidale, C.R. and Milnes, A.R., 1978. Characteristics and origins of some Australian silcretes, tm T. Langford- Smith (Editor), SILCRETE IN AUSTRALIA, Dept. of Geogr., Univ. of New England, Armidale: 20-39. Langford-Smith, T., 1978. SILCRETE IN AUSTRALIA (Editor), Dept. of Geogr., Univ. of New England, Armidale. Mason B., 1966. PRINCIPLES OF GEOCHEMISTRY. 3rd Edition. John Wiley §& Sons Inc., New York. SeniOr, bok. L9/S.— ollcrete and chemically weathered sediments in southwest Queensland, tm T. Langford-Smith (Editor), SILCRETE IN AUSTRALIA, Dept. of Geogr., Univ. of New England, Armidale: 41-50. R.A Glen Geological Survey of New South Wales, Department of Mineral Resources, Box 5288 GPO Sydney, N.S.W. 2001 Australia. J.T. Hutton 12 Bellevue Pl., Unley Park, S.A. 5061, Australia. omale, D., 1973. Sileretes. and associated Silica diagenesis in southern Africa and Australia. 7. Sediment. Petrol. , 43, 1077-1089. Stephens, C.G., 1971. Laterite and silcrete in Australia. Geoderma, 5, 5-52. .Wasson, R.Jo, Hunt, P.A. and Clarke, M.F., 1979. A re-evaluation of the 'silcretes" of the Cobar area, Australia. Geoderma, Zoe VST=159. Watts, S&.H., 1977. Major element geochemistry of silcrete from a portion of inland Australia. Geochtm. Cosmochim. Acta, 41, 1164-1167. Watts, S.H., 1978. The nature and occurrence of silcrete in the Tibooburra area of northwestern New South Wales, 7” T. Langford- Smith (Editor) SILCRETE IN AUSTRALIA, Dept. of Geogr., Univ. of New England, Armidale: 167-1185. Woptner, H., 91978. ‘silcretes of northern South Australia and adjacent regions, 7” 1, Langford-Smith (Editor), SIPLCRETE IN AUSTRALIA, Dept. of Geogr., Univ. of New England, Armidale: 93-141. (Manuscript received 18.1.83) (Manuscript received in final form 6.4.83) Journal and Proceedings, Royal Society of New South Wales, Vol. 116, pp. 25-32, 1983 ISSN 0035-9173/83/010025 — 08 $4.00/ 1 Basement/Cover Relations and a Silurian, I-Type Intrusive from the Cobar Lucknow Area, Cobar, New South Wales R. A. GLEN, G. L. LEWINGTON AND S. E. SHAW ABSTRACT. In the Cobar Lucknow area, 10km NE of Cobar in central western New South Wales, the Wild Wave Granodiorite is intrusive into the Cambro-Ordovician Girilambone Group and is nonconformably overlain by fossiliferous rocks belonging to the Meryula Formation of the Early Devonian Cobar Supergroup. A biotite Rb/Sr age from the granodiorite is 418 + 2Ma [Middle-Late Silurian]. This date is similar to other biotite Rb/Sr ages obtained from other granitoids in_the Girilambone - Wagga Anticlinoral Zone. The Wild Wave Granodiorite has a low initial ®’Sr/®®sr ratio of 0.7051 + 0.002 and is to date the only Silurian I-type granitoid recognised north of the Lachlan River in the Girilambone-Wagga Anticlinoral Zone. Other bodies - the Thule and Erimeran Granites, the Nymagee Igneous Complex, and possibly the Tinderra Granite - are all S-type. From the low initial ratios and the range of Rb/Sr ratios of possible source rock compositions, the source of the Wild Wave Granodiorite is inferred to be from mafic rocks in the lower crust. INTRODUCTION Rocks around the town of Cobar in central western New South Wales consist of a cover sequence, the Early Devonian Cobar Supergroup, and a base- ment sequence comprising the Cambro-Ordovician Girilambone Group and intrusive Silurian granit- oids (Pogson §& Felton, 1978). Although relations between basement and cover are well understood on a regional scale there are very few individual localities where unconformable or nonconformable relations can be clearly demonstrated. Diamond drilling at the Cobar Lucknow Prospect, l10km NE of Cobar, by Getty 0il Development Co in 1980 has enabled us to clarify relations at such a previously, poorly understood site. We can now document the presence here of a Silurian I-type granitoid —the first found north of the Lachlan River in Girilambone - Wagga Anticlinorial Zone of Scheibner (1976) —which is nonconformably overlain by a fossiliferous cover sequence belonging to the Cobar Supergroup. REGIONAL GEOLOGY Relations north of Cobar township are shown in figure 1 (inset). The north/south trending Rookery Fault (RF in figure 1) marks the eastern margin of the Cobar Basin. Rocks to the west are turbiditic in character (Glen, 1982) and belong to the Nurri and Amphitheatre Groups of the Cobar Supergroup. Rocks east of this fault consist not only of basement rocks, low-grade, dominantly turbiditic Ballast beds of the Girilambone Group, but also of infolded outliers of the shelfal Meryula Formation of the Cobar Supergroup (see below) which is equivalent in time to the Nurri Group and lower part of the Amphitheatre Group. Northeast trending linears of the Cobar-Inglewood Lineament (Scheibner, 1973) bracket the Cobar area and are shown in Fig.1 (inset). GENERAL GEOLOGY OF THE COBAR LUCKNOW AREA The geology of the Cobar Lucknow area is dominated by an outlier of the Meryula Formation, which is faulted on its eastern side against low grade Ballast beds of the Girilambone Group (Fig.1). The lack of solid outcrop in the area, and the restriction of exposures to chips and rubble lying on the surface, account for the lack of structural data in figure 1, and also explain differences in previous interpretations. The presence of cover rocks in the Cobar Lucknow area was first noted by Andrews (1913, p 183) and subsequently by Sullivan (1950) and Rayner (1969). Baker (1977, 1978) more recently mapped the outlier as undifferentiated Cobar Group (now Cobar Supergroup), noted its faulted eastern margin, and established a sequence of conglomerate passing up into fossiliferous mud- rock. Subsequent work further south established the presence of several similar outliers to which the name Meryula Formation was given, superseding, in part, the old name Mallee Tank Beds (Pogson § Felton, 1978). Here, we extend the term Meryula Formation to the outlier in the Cobar Lucknow area. The boundaries of the outlier in figure 1 are based on mapping by Lewington (1980), who extended westwards the area of cover rocks recognized by Baker (1977). At the eastern edge of the outlier, conglomerate at the base of the Meryula Formation is faulted against rocks of the Girilambone Group (both unsilicified and silicified) and also occurs in fault slivers surrounded by silicified rocks of the Girilambone Group. On the western side, the outlier is separated by a thin strip of Girilambone Group from another dominantly mudrock cover sequence centred on Maryantha Home- stead. Baker correlated this sequence with the Chesney Formation. However, while not being able to rule out this correlation, we suspect that this second outlier may also consist of Meryula Formation, and show it as such in Fig. l. R. A. GLEN, G. L. LEWINGTON AND S. E. SHAW LEGEND: Alluvial Deposits C7 Great Cobar Slate Ct Ferricrete Try CSA Siltstone NURRI GROUP , CHESNEY FORMATION Sandstone , siltstone , mudstone for other units - see ra eens KOPYJE GROUP, MERYULA FORMATION 7 Linears of Cobar - Inglewood Lineament To Bourke wf (DETAILED ABOVE) Mudstone | siltstone , sandstone ¥| 7 Conglomerate , sandstone eo To Wilcannia 7 WILD WAVE GRANODIORITE (subcrop only ) GIRILAMBONE GROUP (Ballast beds) Undifferentiated Silicified sandstone Approximate geological boundary : EAST Fe | oe F Fault , definite , inferred = Cover Se creseat RF— ————RF Rookery Fault LL feo poe ated sti +>: — > ss Anticline , syncline with plunge A ae ee mes Ae,Be,Ce Fossil localities ~ SCHEMATIC SECTION : bd Ach Orllt poles LUCKNOW OUTLIER RL, Rw Mines , Cobar Lucknow , Wild Wave —_—_———— Road , track BIG. J Locality Map (inset) and Map of the Cobar Lucknow Area, showing location of the Wild Wave Granodiorite. Schematic cross section also shown. COBAR LUCKNOW AREA | Two diamond drill holes sunk near the Cobar Lucknow group of shafts by Getty 011 Development Co in 1980 to test co-incident aeromagnetic, gravity, I.P. and soil geochemical anomalies, penetrated fresh granodiorite. Presence of fresh granodiorite in drill core explains weathered samples on the dump of the main Cobar Lucknow shaft, first noted by Mulhol- land (pers. comm. to Sullivan, 1950). Both Sullivan (1950) and Rayner (1969) inferred the presence of subsurface granite in this area, Rayner calling it the Wild Wave Granite, which we now amend to Wild Wave Granodiorite. Baker (1978), however, noted the presence of cobble-size fragments of weathered granite and wondered whether they merely indicated the presence of granite conglomerate. As will be described below, both WELEWS are COrrect. DESCRIPTION OF GEOLOGICAL UNITS Girilambone Group (Ballast beds) Lithologically, the unit consists of micaceous sandstones, cleaved mudstones and discontinuous chert beds. Some fragments of sandstone contain planar and cross lamination. Bands of en echelon quartzite lenses, especially west of the Cobar Lucknow shafts, may reflect shear zones. Around the shafts themselves, sandstones are silicified in a 100m wide zone which fringes both the southern and eastern sides of the granodiorite. Wild Wave Granodiorite The granodiorite does not outcrop, but is concealed beneath recent cover and Devonian sediments. The inferred subcrop of this granod- iorite, shown in figure 1, is based on drill intersections coupled with aeromagnetic and gravity anomalies. The rock is generally grey in colour, medium grained and massive with no obvious mineral orientation. Samples taken from three section of granodiorite in hole CL1-Gl (100.00-160.85 m), G2 (108.65-199.00 m), G3 (228.5-228.9 m)-are dominated by quartz, sub- hedral plagioclase well twinned and zoned, interstitial K-feldspar, some microperthite, hornblende and biotite. Accessory minerals include apatite, magnetite and zircon. Biotite and hornblende occur as discrete crystals (2-4mn), commonly poikilitic, and also as intergrowths with biotite replacing hornblende. Alteration minerals consist of chlorite after biotite, epidote, sphene and carbonate from hornblende, andi minor Wservcice’ ater feldspar (see Appendix 1). The aeromagnetic anomaly of 85y over the pluton confirms the presence of moderate amounts of magnetite. Talc and chlorite-filled fractures are also common. Cross-cutting veins of calcite also contain small amounts of pyrite, pyrrhotite, galena and chalcopyrite. These sulphides are presumably responsible for the IP and geochemical anomalies identified during the early exploration phase. Table 1 lists the chemical compositions of samples Gl, G2 and G3. The analyses show a restricted range of silica around 64 percent and are reasonably high in K,0, reflecting high modal biotite. Sr values are high, a characteristic of the shoshonite I-type granitoids e.g. the Moonbi Plutonic Suite (Shaw § Flood, 1981), and are much higher than the I-type plutons Of the Berridale Batholith (White et al, 1977). The Wild Wave Granodiorite has distinctive I-type characteristics of Chappell §& White (1974) and is unlike the A-type granitoids (Collins et al, 1982) which are characterised by much higher Si02 and greater abundances of the highly charged cations such as Y and Zr. Meryula Formation The basal unit recognized in this formation in the Cobar Lucknow area is a conglomerate which outcrops generally only around the margins of the outlier (Fig.l). Maximum outcrop width of the conglomerate occurs along the eastern side of the outlier, against the bounding faults, and the conglomerate was probably deposited as a continuous sheet, now partially removed by erosion, from north of the Cobar Lucknow group of shafts to south of the Woolshed. From this part of the outlier, the conglomerate thins to the west, where it is restricted to minor lenses only. Around the Cobar Lucknow group of shafts, data obtained from the two drill holes and also from a partial descent of the main shaft indicate that conglomerate overlies a 20-50m thick zone of weathered granite. The boundary between the two is difficult to pick. Conglomerate up to 50m thick, contains pebble to cobble-size fragments of chert, siltstone, feldspar, quartz and granodiorite. Towards the top of the main Cobar Lucknow shaft, beds of conglomerate alternating with beds of arkosic sandstone dip at low angles (15°-20°) off the granodiorite to the northeast. Elsewhere in the outlier, basal conglomerate passes upwards into a mudrock sequence which contains beds of sublithic arenite, up to Im thick. Sandstones vary from massive to planar and cross laminated. Baker (1978, p35) reported a typical composition as 80% quartz grains with detrital muscovite in a groundmass consisting of quartz plus "sericite'’. Mudrocks weather to purple or yellow- brown in colour and outcrop badly. They are poorly cleaved. Fossils have been found from five localities in the outlier. Those reported by Baker (1978), (Fig.1, locality B), include various brachiopods and corals indicative of an Early Devonian age (Sherwin, 1974). Other fossils include crinoid stems (locality C), trilobites and brachiopods (locality D) of an age near the Siluro-Devonian boundary, brachiopods with cephalopods (locality F) (Sherwin, 1980a), and brachiopods from locality A Fig.l] which are Early Devonian in age (Sherwin, 1980b). (See Appendix 2). DATING OF THE WILD WAVE GRANODIORITE Concentrates of biotite from two samples of drill core from hole GLl were separated and dated using Rb/Sr techniques and precisions (Shaw et al, 1982) at the CSIRO Division of Mineral Physics, North Ryde. Ages were calculated using biotite-bulk rock pairs. An average of four runs on Gl biotite gave an age R. A. GLEN, G. L. LEWINGTON AND S. E. SHAW TABLE 1 CHEMICAL ANALYSES WILD WAVE GRANODIORITE DIAMOND DRILL CORE SPEC. NO. Gl G2 G3 Sid, 63.99 64.14 64.14 Ti0, 0.63 0.61 0.59 Al,0. 15.76 16.06 15.60 re) Fe,0, 1.15 1374 1241 Feo Be Dl 2.94 3.04 MnO 0.06 0.06 0:07 MgO O78 3.83 2.35 CaO BOT 4.26 4.03 Na,,0 2o79 2.85 2282 K,0 3.73 3.08 3.40 P0. 0232 0.30 0.30 H,0° 0.99 1.02 1.53 HO Ona 0.10 0.10 Nb 22 2) 2G, zr 150 161 153 Y 19 28 26 Sr ake 768 747 Th 13 19 15 Pb 4 2 5 U <2 <2 <2 Rb 165 129 144 Zn 38 46 46 Cu Li: 14 13 Ni 7 7 6 Cr 31 30 36 V 99 101 103 Ba 811 730 759 CALCULATED MODE* *BASED ON THE COMPOSITIONS OF HORNBLENDE AND BIOTITE FROM THE SOUTHERN PART OF THE NEW ENGLAND BATHOLITH (MOONBI NORM OF B.W. CHAPPELL, PERS. COMM.). SPEC< NO. Gl G2 G3 QUARTZ 24.1 25.6 25,22 PLAGIOCLASE 57 30 40.8 589 K-FELDSPAR S59 80 i229 BIOTITE WORZ 20.8 17.4 HORNBLENDE 4.2 Sa) 4.6 APATITE OS 0.5 0.5 MAGNETITE Oz9 0.5 OS COBAR LUCKNOW AREA of 419.0 + 1.5 Ma. Two runs on G2 biotite gave an age of 416.0 * 0.8 Ma (Table 2). Because of the: possibility of radiogenic Sr loss, the estimates are minimum ages only, although the lack of deformation (other than very minor biotite kinking) and regional metamorphic effects suggest the biotite ages represent the time of emplacement and crystallisation. Initial &/Sr/ 86Sr ratios based on biotite bulk rock pairs on samples Gl and G2, average 0.7051 (Table 2). TABLE 2 ISOTOPIC DATA, WILD WAVE GRANODIORITE Rb (ppm) Sr (ppm) 87Rb/86Sr BLOtiate Data* Spec. No. Gl SOS 23.64 74.8817 Dupl 1.Gl 593.13 25062 75.9309 Dupl 2.G1 589.90 23.18 76.9921 Dupl 3.G1 589.86 26.43 67.1590 G2 393.96 36.41 5128199 Dupl 1.G2 392.49 S0eaS SO 70590 Rock Data Spec. No. Gl 165 714 0.66934 G2 129 768 0.48644 oe calculated from biotite-bulk rock pair. Initial BUG) Sr ratios Gi =-0),70527 G2 = 0.70501. 87Sr/®8°Sr(p.d.) i L5Z205 {15670 1.16446 alO7e9 Av 0239329 0.93363 Av 0.70926 0.70790 Age (Ma) 418. Aly. 418. 420. 419. 415. 416. 416. 44 DL Unspiked 875r/86Sr of SRM 987 gave Biotite separates were prepared by rolling and sieving. Coarse-grain size (+80 mesh) and apatite inclusions mean). probably account for variations in the values of Sr. N87Rb = 1.42-x 10 “1! re Normalised to ®6Sr/®88Sr = 0.1194. 0.71036 +0.00011 (standard error of the 29 Errors in biotite Rb and Sr determinations based on replicate analyses of NBS 607 K feldspar are estimated to be less than The average age of Gl and G2 combined is 418 + 2 Ma 0.2% (standard error of the mean %). 30 R. A. GLEN, G. L. LEWINGTON AND S. E. SHAW CONCLUSIONS As outlined above, nonconformable relations in the Cobar Lucknow area occur between sediments of the Early Devonian Meryula Formation and the underlying Silurian I-type, Wild Wave Granodiorit which is intrusive into the Ballast beds of the Girilambone Group. Sample G2 (416.0 + 0.8 Ma) is slightly younger than sample Gl (419.0 + 1.5 Ma). If real, this difference may reflect the greater alteration. of biotite to chlorite\in sample G2. The average biotite Rb/Sr age of the Wild Wave Granodiorite of 418 + 2 Ma (combining Gl and G2) is interpreted to be a minimum age representing the time of cooling after high level emplacement. Taking the base of the Silurian as 436 Ma (Lanphere et al, 1977), and the base of the Devonian as 410 Ma (Armstrong §& McDowall 1975, Owen § Wyborn 1979,Richards et al, 1977), this date falls around the boundary between the Middle and Late Silurian. The age data on the Wild Wave Granodiorite can be compared with data from other Silurian granitoids in the Girilambone-Wagga Anticlinorial Zone. North of the Lachlan River, the oldest minimum age for the Thule Granite (K/Ar on biotite) is 422 + 6 Ma. Pogson §& Hilyard (1981) estimated a maximum age of 440 Ma for the foliated phase of the Nymagee Igneous Complex. South of the Lachlan River, the Kikoira Granite gives a corrected* K/Ar age of 417 + 3 Ma (Richards et al, 1982). These latter authors also report ages of 417 + 2.5 Ma (Rb/Sr mica concentrate) on the Mine Granite at Ardlethan and 410 + 2.5 Ma (Rb/Sr and K/Ar) on the Ardlethan Granite. Geochemical identification of the Wild Wave Granodiorite as an I-type intrusive is supported by the identification of hornblende and magnetite, the latter also reflected in the geophysics. With the exception of the I-type Tibooburra Granxte with a K/Ar biotite age around 403 Ma (Evernden & Richards 1962, corrected to new constants) and a Rb/Sr biotite age around 410 Ma (Shaw § Flood, 1982), the Wild Wave Granodiorite lies further west than most of the I-type granitoids recorded from N.S.W. To date this body is the only Silurian I-type body identified in that part of the Girilambone-Wagga Anticlinorial Zone lying north of the Lachlan River: the Nymagee Igneous Complex, Thule Granite and Erimeran Granites are all S-types (Pogson, 1982), as may be the Tinderra Granite. Based on the models of Chappell §& White (1974), this difference in granite types retlects, differences in melt source material; the I-type being generated by melting of an igneous source, the S-type from melting of a sedimentary source. Pogson (1982) noted that the Thule and Erimeran Granites and the Nymagee Igneous Complex are low Ca granites in the sense of Fagan (1979), and suggested that they formed by partial melting of the quartz-rich, Ca-poor rocks of the Girilambone Group. The age of the Wild Wave Granodiorite source rock material can be calculated, providing *corrected for new international constants as used by Steiger & Jager .(1'977). assumptions of Rb/Sr and initial ®8’Sr/®8®Sr are made. Compston §& Chappell (1979), in a study of granitoids of the southern part of the Lachlan Fold Belt, calculated source rock Rb/Sr compositions varying from 0.066 to 0.22, and initial 87Sr/®6Sr ratios varied from 0.7031 to 0.7042. Alternatively, source compositions can be estimated from the extra- polation of modern day island are volcanics. Typical Rb/Sr ratios vary from 0.02 to 0.08, and 87Sr/86Sr ratios average 0.7037. On a mantle growth curve, the ®7Sr/86Sr ratio would extrapolate to approximately .7031, at between 1000 Ma and 1200 Ma. Thus assuming a source Rb/Sr ratio of 0.066, and an initial 87Sr/®€Sr ratio of 0.7031, equivalent to the lowermost values of Compston § Chappell (1979), the age of the Wild Wave Granodiorite source would be 1100 Ma, similar to that calculated by Compston § Chappell for source material of their "non-minimum-melt" granitoids. This calculated source age is considered to be a maximum only, and on this basis would correspond to a Proterozoic rather than a Lower Palaeozoic source. From the granitoid data just discussed, we summarise our conclusions as follows: iE) The period around 420 Ma was marked in the Girilambone-Wagga Anticlinorial Zone by emplacement of large volumes of granitoids. This implies a high heat flow under a large part of this aréa at this time, or just cariluer: 2) Generation of the S-type granitoids at mid crustal levels (Pogson, 1982) implies a high heat source. 3) The I-type Wild Wave Granodiorite probably formed at a deeper level than the S-type granitoids, from a more mafic lower crust. Rise of this melt to its present position was probably accomplished up a major crustal fracture during a period of crustal extension. This would account for the location of the Wild Wave Granodiorite lying within the Cobar-Inglewood Lineament. 4) The low initial ratio of the I-type Wild Wave Granodiorite would suggest that its source material is Upper Proterozoic or younger, similar to that proposed by Compston §& Chappell (1979) for the southern part of the Lachlan Fold Belt. ACKNOWLEDGEMENTS Getty Oil Development Co is thanked for permission to work on the granodiorite core and publish the results. C.S.1.R.0. “Institutevor Earth Resources (North Ryde) is thanked for providing access to their age-dating facilities. D.J. Pogson is thanked for reading the manuscript. Glen publishes with permission of the Secretary, NSW Department of Mineral Resources. REFERENCES Andrews, E.C., 1913. Report on the Cobar Copper and Gold-field, Part I. Mineral Resources, Geologtcal Survey of N.S.W., 17, 207pp. Armstrong, R.L. and McDowall, W.G., 1975. Proposed refinement of the Phanerozoic time scale. Geodynante Highlights 2, 33-34. COBAR LUCKNOW AREA 31 Baker, C.J., 1977. Cobar 1:100,000 Geological Sheet 8035. Geological Survey of N.S.W., Sydney. Baker, C.J., 1978. Geology of the Cobar 1:100,000 Sheet 8035. Geological Survey of N.S.W,, Sydney. Barron, L.M., 1980. Mildly porphyritic biotite hornblende granodiorite basement on Cobar 1:100,000. Geological Survey of N.S.W., unpublished report GS 1980/345. Chappell, B.W. & White, A.J.R., 1974. Two contrasting granite types. Pac. Geol., 8, 173-4. Collins, W.J., Beams, S.D., White, A.J.R. and Chappell, B.W., 1982. Nature and origin of A-type granites with particular reference to Southeastern Australia. Contrib. Mineral Petrol., 80, 189-200. Compston, W., and Chappell, B.W., 1979. Sr-isotopic evaluation of granitoid source rocks tm THE EARTH: ITS ORIGIN, STRUCTURE AND EVOLUTION, McElhinny.M.W., (ed). Academic Press London, 377-426. Evernden, J.F., and Rrchards, J.R., 1962. Potassium-argon ages in eastern Australia. J Geol. Soc. Aust... 9, 1=50. Fagan, R.K., 1979. Deformation, Metamorphism and Anatexis of an Early Palaeozoic Flysch Sequence in Northeastern Victoria. Ph.D. Thesis, U.N.E. Armidale, (unpubl.) Glen, R.A., 1982. The Amphitheatre Group, Cobar New South Wales: preliminary results of new mapping and implications for ore search. Q@.Notes, Geologtcal Survey of N.S.W., 49, 1-14, Lanphere, M.A., Churkin, Jr., M., and Eberlein, G.S. 1977. Radiometric age of the Monogra- ptus cyphus graptolite zone in southeastern Alaska - an estimate of the age of the Ordovician - Silurian boundary. Geol. Mag. 114, 15-24. Lewington, G.L.D., 1980. Report on exploration EL 1310, Cobar Lucknow area, NSW for 6 months ended 14th August 1980. u.L.Gilfillan & Assocs P/L (File Geol. Survey NSW, GS 1980/306) (unpubl.). Owen, M., and Wyborn, D., 1979. Geology and Geo- chemistry of the Tantangara and Brindabella 1:100,000 Sheet areas. Bureau of Mineral Resources - Bulletin 204, S2pp. Pogson, D.J., 1982. Stratigraphy, structure and tectonics: Nymagee-Melrose, central western New South Wales. M.Sc. thesis, N.S.W. Institute of Technology (Sydney) (unpubl.). Pogson, D.J., and Felton, E.A., 1978. Reappraisal of geology, Cobar-Canbelego-Mineral Hill region, central western New South Wales. @. Notes, Geologtcal Survey of W.S.W., 33, 1-14. Pogson, D.J., and Hilyard, D., 1982. Results of isotopic age dating related to Geological Survey Investigations, 1974-1978. W.S.W. Dept. of Mineral Resources, Records 20(2) 2ol=275. Rayner, E.O., 1969. The Copper Ores of the Cobar Region. Memotr, Geologival Survey of WioeWs, 10, iSipp: Richards, J.R., Barkas, J.P... and Vallance, f.Ge. 1977. A lower Devonian point in the geological time scale. Geochem Jnl, 11, L47=1:55.. Richards, J.R., Compston, W. and Paterson, R.G., 1982. Isotopic information on the Ardlethan Tinfield, New South Wales. Proc. A.I.M.M. 284, 11-16. Scheibner, E., 1973. ERTS-Geological Investigations of New South Wales, Geological Survey of N.S.W., unpublished report GS 1973/382. Scheibner, E., 1976. EXPLANATORY NOTES ON THE TECTONIC MAP OF NEW SOUTH WALES. Geological Survey of N.S.W., Sydney 283 pp. Shaw, S.E., and Flood, R.H., 1981. The New England Batholith, Eastern Australia: geochemical variations in time and space. J, Geophys. Res., 86, 10530-10544. Shaw, S.8., and Flood, R.H., 1982. Granitoids of the Lachlan Fold Belt. Geol. Soc. Aust., Abstracts 6, 3. Shaw, S.E., Flood, R.H. and Riley, G.H., 1982. The Wologorong Batholith, New South Wales, and the extension of the I-S line of the Siluro-Devonian granitoids. J. Geol. Soe. Aust., 29, 41-48. Sherwin, L., 1974. Siluro-Devonian fossils from Cobar and Wilgaroon. Geological Survey of N.S.W., unpublished report GS 1974/001. Sherwin, L., 1980a. Fossils from an area northeast of Cobar. Geological Survey of N.S.W., unpublished report GS 1980/1360. Sherwin, L., 1980b. Fossils and trace fossils from the Cobar 1:100,000 Sheet. Geological Survey of N.S.W.,unpublished report GS 1980/206. Steiger, R.H. and Jager, E., 1977. Subcommission of geochronology: convention on the use of decay constants in geo-and cosmochemistry. Hartn Planet Ser. Letet., 36, 359-362. Sullivan, C.J,, 1950. Mineralization in the Cobar- Nymagee province, and its significance. Proc. A.I.M.i4., 156-157, 154-176. White, A.J.R., Williams, I.S. and Chappell, B.W., I977~— Geology of the Berridale 1:100,000 Sheet 8625. Geological Survey of N.S.W., Sydney. by R. A. GLEN, G. L. LEWINGTON AND S. E. SHAW APPENDIX 1. Petrography of the Wild Wave APPENDIX 2. Palaeontology Granodiorite (based on observation and part from Barron, 1960). Locality A Brachiopods ?Atrypa sp. (poorly preserved) Gl. quartz-feldspar-hornblende-biotite granodiorite Early Devonian Quartz (24%, 0.6-0.8mm) slightly stained with Sherwin (1980a). undulose extinction and minor bulging along quartz/quartz and quartz/feldspar boundaries. Locality B Brachiopods. ?Plectatrypa sp. Plagioclase (40%, 0.3-1.7mm) subhedral, well 9? twinned and concentrically zoned. Minor 2Cent one tia replacement by “sericite". K feldspar ?Schizotreta sp. (14%, to 3mm). Some microperthite. Hornblende (4%, 0.8-1.4mm) pale green-yellow subhedral- Indet. dalmanellids, anhedral grains up to lmm. Minor alteration rhynchonellids, strophomenids to carbonate, ?sphene and chlorite. Poikilitic with inclusions of quartz and feldspar. Good Corals ? Alveolites sp. equilibrium texture. Also occurring as inter- Early Devonian (7?) growths with biotite, with biotite probably Sherwin (1974a) ,Baker (1978 App.1) replacing some hornblende. Biotite as above and also(15%, 0.4-2mm} discrete subhedral to Locality C Crinoid stems (large) anhedral grains. Inclusions of quartz and Sherwin (1980b) needles of ? rutile. Random preferred orientation. Some bending of (001) traces Locality D Trilobites Encrinurus_ sp. and some alteration and opening along (001). oGpayicalmenes Alteration to chlorite in places. Minor eee Mel SDUERS CPLGOEe; .2u econ = apauyEcaane Brachiopods indet. stropheodontids magnetite. Early Devonian G2. as above. Biotites more altered to chlorite, (Shermim q(1980b) and more magnetite. Good evidence for some biotite replacing hornblende. Rock frag- : aie L i 1 1 i Ee ee ep ocality E Echinoderm debris (Sherwin (1980b) G3. as Gl. Biotites less altered than those in G2; more like Gl. Magnetite like G2. Good equilibrium textures between hornblende (to 4mm), quartz and feldspar. Magnetite associated with hornblende and biotite. Locality F Brachiopods indet. ?strophomenids Cephalopods orthoconic, nautiloids Early Devonian Sherwin (1980b) Locality G Trilobites Gravicalymene Brachiopods ?Protochonetes_ sp. ?Howellella = sp. Cephalopods Michelinoceras sp. Tentaculitids Nowakia cf acuaria (Richter) ?Tentaculites = sp. Early Devonian Sherwin (1974), Baker (1978 App.1). Glen’, Rene: eninecones G.L., and Shaw, S.E. 1. Geological Survey of New South Wales, Box 5288 GPO Sydney, N.S.W. 2001. 2. Getty 011 Development Co., P.O. Box 1407, North Sydney, N.S.W. 2060. 3. School of Earth Sciences, Macquarie University, North Ryde, N.S.W. 2113. (Manuscript received 18.2.83) (Manuscript received in final form 18.4. 83) Journal and Proceedings, Royal Society of New South Wales, Vol. 116, pp. 33-40, 1983 ISSN 0035-9173/83/010033 — 08 $4.00/ 1 Astrometric Determination of Mass Segregation and Membership Probabilities in Galactic Clusters DAVID S. KING ABSTRACT. Using positional as well as proper motion information allows a more reliable determination of the membership probabilities in the region of galactic clusters. Applying a positional fit to cluster members indicates that the more massive stars congregate towards the cluster centre in NGC 6087 and NGC 3532. INTRODUCTION In a previous paper (King 1979), a method was described whereby a probability of membership could be assigned to stars in the region of a galactic cluster. This probability was calculated on the basis of proper motion only. The inclusion of positional information gives a more reliable membership proba- bility and allows a test to be made to ascertain if the more massive cluster stars congregate towards the cluster centre. THE PROBABILITIES The method described in the previous paper (King 1979) was devised by Sanders (1971) and involved representing the observed proper motions as two overlapping bivariate gaussian frequency functions. Using the maximum likelihood method enabled the seven parameters in the distribution equation to be esti- mated. The drawback with this method was that it gave high probabilities of membership to stars with Similar proper motion to the cluster no matter how far they were from the cluster centre. Incorporating positional as well as velocity information into the distribution equation offers twice the information at the expense of five extra parameters. It is assumed that the field stars are uniformly distributed over the area studied and the cluster stars are distributed in three dimensions like a poly- trope of index five. A polytrope of index five (Plummer's model) consists of a finite distribution of mass which is infinite in extent. Seen in projection, Plummer's model obeys the following density equation with r being the distance from the centre and R the radius containing half the mass in projection. Te I NO | ues Be R° L Resear ar Plummer (1911) was the first to suggest that globular star clusters obeyed this distribution law. More recently, it has been used as the starting model for computer simulation of star clusters. Combining Plummer's model with the proper motion distribution model gives the following distribution equation:- a( ee ne Hp 9Ve orbs ony - + Ne 1 (i (v,-¥,)* = exp - 3 + z OnE LA 2 r re ay, x y =o 2 , 2 2 ‘ : . (E.-6)) . ty ote? a 1 (u,-X) + Ot Pep 2 2 ~ 2 2 R_R R R 2 Been E n °¢ Ne eee uf? 18 . 22 34 DAVID S. KING The unknowns in the distribution equation are o_, the dispersion of the cluster star motions; N,, N the number of field and cluster stars; X,, Y, the cefitre of the field star proper motion distribution; X_, Y_ the centre of the cluster star proper motions, previously assumed to be zero; =, 2 the field star proper motion dispersions; &._, 4 the cluster centre and R_, Ry the cluster radii containikg half the mass in projection. There are an additional two unknowns; 0 the rotation angle of the observed proper motions (+ to +v) into a new coordinate system defined by the principal axes of the apparent ellipsoidal distri- bution of field star motions; and yp the rotation angle of the positions (+& to +n) into new positional coordinates defined by the principal axes of the cluster. The positions &., n. and the velocities y., v. are then obtained in their new coordinate systems. A is the area for which positions and velocities are known. Cc The method of maximum likelihood then gives the following non-linear equations of condition:-— 1 a vB Ne $ ) — ener Sears = 10 o/ £5 A o_R_R xX y c — n a Xe : 7" uj;-Xp =) = oe Ye 5 ) A v “Y> = 0 8 Cu, -%,)* xy : — 5 - j =" ® z X a (v,-¥,)° hie p —_— - 1 = 0 y o i ree a i Nea | vy Cuy-Xp) : uw; vy-Yp? r NO MGE aan ne ball Bare A 5° 5° TooHR ie x y X y c Een c MASS SEGREGATION AND MEMBERSHIP 35 1.65 BY nm 3 pa ; Neate = 0 3) 2 YB Yy (Si=Sc) Ro: a = ti = 0 E VE, Ro E 78 4y Gres Re ese pale = = = 0 n 3 Ro n ed - i By n(&.-E) ; E(n,-n,) an 2 |e The summations being over the known total population (N +N, - The previous 14 equations are solved by assuming initial values then calculating the value of each parameter in turn. After several iterations the parameters converge in most cases. Thus, the probability of membership is determined for star i as:- Field stars which fail to fit the gaussian field star distribution due to local motion and differential galactic rotation are pruned one at a time until the distributions, given by proper motion only, reach their best fit. This method gives two probabilities of membership, the first using only the proper motions and the second using proper motion and positional information. CASE STUDY OF NGC 6087 The above procedure for obtaining two membership probabilities was applied to the galactic cluster NGC 6087 (King 1982). It was found that the nine parameters in common to both types of distribution function were in reasonable agreement, although the number of field stars increased with the inclusion of positional information. This was to be expected for the reason given earlier, that field stars with cluster type motion were previously given cluster status no matter how far they were from the cluster centre. To illustrate the effect that positional parameters have on the membership probabilities, the following diagrams were produced. Diagram A is the proper motion plot for stars with motions less than 1.4 seconds of arc per century. It can be easily seen that it is composed of two binormal distributions. One distri- bution is circular centred on zero which represents the cluster stars all moving together. The other dis- tribution represents the field stars and is elliptical, more extensive and has its major axis at 36 degrees to the right ascension axis. It is by resolving stars into these two components that the probabilities based on proper motion are derived. Diagram B shows us the positional information we have available for stars in the region of NGC 6087. The star at position (100.0, 100.0) is at right ascension 16 14 4072 and declination -57° 47' 138. The axes are in millimetres and one millimetre represents one second of arc. When only the stars with proba- bilities of membership greater than 90% are plotted, diagrams C and D are produced. Diagram C gives the positions of 65 stars with membership probabilities greater than 90% based on proper motion only. Diagram D gives the positions of 47 stars with membership probabilities greater than 90% based on position as well as proper motion. Diagram D has excluded stars from membership that lie a long way from the cluster centre as well as included some extra stars close to the cluster centre. CASE STUDY OF NGC 4755 Membership probabilities were also determined for the galactic cluster NGC 4755 using both methods. Previously only probabilities using proper motions were published (King 1980). Diagram E shows the field stars in the region of the cluster on the basis of proper motion. Diagram F was obtained by using proper motion as well as position to find the non-members. The difference between the two diagrams is a striking 36 POSITION IN DEC. 100.00 140 60.900 DAVID S. KING DTAGPAM A Oo Wo O64 N z _— z2 oF — O i ro) = (=) (o} Q wo { (=) QoQ (=) (o>) T (o) QO (o) vw At = "140.00 -100.00 -60.00 -20.00 20.00 60.00 100.00 140.00 MOTION IN R.A. nN * # * DIAGRAM B =) * : . . * 2K 2 a ye mK * * ¥ y * * . ro) * Ay * 2 % ° ~ % x * 2 * = * * * ~ * * a : =) KK *% nm * **K * ‘al * oO Me * ¥ = * * Ss % * * * ¥€ 3 Se * * *K * o mk > * eek * mK % * * 2 * * * KR * * ¥* vn %* * * (oo) lo) a (=) (o) w eo (o} [o) a “79.90 85.00 91.90 97.00 103.900 109.00 115.00 121.00 POSITION IN R.A. MASS SEGREGATION AND MEMBERSHIP 121 DIAGRAM Cc 115.00 * 97.00 103.00 109.00 POSITION IN DEC. -00 91 85.00 ro) (o>) 2 79.00 85.90 91.00 97.00 103.00 109.00 115.90 < POSITION IN R.A. o °o w DIAGRAM D my 8 , . o * * Oo e x * ws x QF: * x * © > x* * = * *y * * * * z= * * a «* mee ye * . * =f * aie al is x wn? oO Qa ° ° a °o ° wo oo (oe) ° o nK 79.00 85.00 91.90 97.00 103.00 POSITION IN R-A. 109.00 115.00 121.00 Sig) 121.00 38 POSITION IN DEC. 97.00 103.00 109.00 115.00 121 91.00 85.00 79.00 79.00 DAVID S. KING 21 | 115.00 109.00 POSITION IN DEC. -00 91 85.00 79.00 85.00 103.90 97.00 79.90 85.00 91.900 eas 91.00 97.00 97 DIAGRAM E I3-00 POSITION IN R.A. 103.00 109.00 POSITION IN R.A. DIAGRAM F 115.00 109.00 115.00 121.00 121.00 MASS SEGREGATION AND MEMBERSHIP Shy, example of the discrimination of the new method. Diagram E obviously has some stars left in it which are members, whereas diagram F appears to be a random distribution of field stars. This difference in the appearance of field stars was also present in NGC 6087, but did not appear so clearly. MASS SEGREGATION Because of the positional information given by the additional parameters in determining the new probabilities, it becomes possible to make a quantitative estimate of the diameter of the cluster. For NGC 6087, 78 members on the basis of position and velocity were selected. Using the method of maximum likelihood, the five parameters relating to positional information were obtained. The value of Re 2s 618 and Ry is 8!4. The 78 members were divided into two different magnitude ranges, one between magnitudes 7.5 and 10.6 and the other between 10.6 and 11.1. The average magnitude in the first group is 9.95 and in the second group is 10.9. Assuming the distance to NGC 6087 is 910 pe (Landolt 1963), then these magnitudes correspond to solar masses of 3.6 and 2.5 respectively. The 39 bright members gave the value of Ry as 6!3 and Ry as 7!2. The 39 faint members gave the value of Re as 7!2 and Ry, as 9!6. This provided some evidence of mass segregation of the heavier stars towards the cluster centre as predicted by the computer simulation of clusters. However, the number of stars is insufficient to draw any firm conclusion, so a previously studied cluster NGC 3532 (King 1978) was examined. Using the method already described, 237 members were selected. The results are in Table 1. Table 1 -—- Radius of NGC 3532 237 members 118 bright members 119 faint members Re 10:4 9°9 1016 Ry Bue 619 O25 The 118 bright members have an average magnitude of 9.12 which at 430pe (Schmidt 1963) corresponds to 2.7 solar masses. The 119 faint members have an average magnitude of 10.52 corresponding to 1.9 solar masses. This provides a strong indication of mass segregation in galactic clusters. LIST OF DIAGRAMS DIAGRAM A Proper motions in the region of NGC 6087. Motions of stars in right ascension (R.A.) and declination (DEC.) are in units of O"01 per century. DIAGRAM B - Stars in the region of NGC 6087. ee 6. anh A Positions of stars are shown with (100.0, 100.0) corresponding to R.A. 16 14 40.2, Dec. -57 47' 13"8. The axes are in millimeteres and one millimetre represents one second of arc. DIAGRAM C -— Members of the cluster NGC 6087 using proper motion. Positions of cluster members with probabilities of membership greater than 90% based on proper motion only are shown. DIAGRAM D — Members of the cluster NGC 6087 using positional and velocity information. Positions of cluster members with probabilities of membership greater than 90% based on proper motion and position are shown, DIAGRAM E —- Field stars in the region of NGC 4755 on the basis of proper motion. Positions of non-members with probabilities of membership less than 50% based on proper motion only are shown. DIAGRAM F —- Field stars in the region of NGC 4755 on the basis of positions and velocities. Positions of non-members with probabilities of membership less than 50% based on proper motion and position are shown. CONCLUSION Provided a large area is examined surrounding a galactic cluster, and all stars are examined down to a fixed magnitude limit, it is possible to obtain a clear distinction between cluster and field stars by taking into account both proper motion and positional data. Cluster members determined in this manner may exhibit mass segregation of the heavier stars toward the cluster centre. Further examination of the mass segregation may be used to compare models of cluster evolution. ACKNOWLEDGMENTS The author wishes to acknowledge the support of the University of Sydney on whose computer the mem- bership models were calculated as contribution toward a Ph.D. thesis entitled "Open Cluster Dynamics; a Comparison of Theory, Simulation and Observation", 40 DAVID S. KING REFERENCES King, D.S., 1978. ed. Roy. Soc. N.S.W., 111, 1-12. King, D.S., 1979. ¢« Roy. Soc. N.«S.Ws, 1172, 101=104. King, D.S., 1980. <. Hoy. Soc. NeS.W.; 176, 65-68. King, D.S., 1982. od. Hoy. Soc. N«S.We, 115, TH. Landolt, A.U., 1963. Ap. J. Supp., 8, 329-351. Plummer, H.C., 1911. Mon. Not. Roy. Astron. Soc., 71, 460-470. Sanders, W.L., 1971. Astronomy and Astrophystes, 14, 226-232. Schmidt, J., 1963. Astron. Nachrichten, 287, 41-48. Sydney Observatory, Observatory Park, SYDNEY. N.S.W. 2000 (Manuscript received 10.6.1983) REPORT OF COUNCIL FOR THE YEAR ENDED 3lst MARCH, 1983 4] MEETINGS Council held 11 meetings during the past year. Attendance of members of Council ranged from 10 to 14. Nine general monthly meetings were held dur- ing the year together with the Liversidge Lecture delivered by Professor D.P. Craig on ''Molecular Crystals and Light: Chemical Reactions in Cages" on 20th May, 1982 at Macquarie University. Abstracts of the lectures at the monthly meetings have been published in the Society's Newsletter. The average attendance at the general monthly meetings was 24. (range 17 to 35). ANNUAL DINNER The Annual Dinner was held at the Great Hall of the University of Sydney on Wednesday, 2nd March, 1983, and 91 members and guests were present. We commemorated the centenary of the Faculties of Medicine and Engineering of the University of Sydney, and Professor J.M. War, the Vice-Chancellor and Principal gave the address. PUBLICATIONS Volume 115, Parts 1 to 4, of the Journal and Proceedings were published during the year. There were 10 issues of the Society's Newsletter. Council is most grateful to the authors of short articles which are much apprec- iated by members. MEMBERSHIP The membership of the Society at 31st March, 1983 was: Honorary Members 12 Life Members 55 Company Member 1 Ordinary Members 527 Associate Members 40 LIBRARY There were a total of 98 requests for photocopying from the library during the year. Of these 9 requests were from members, and the remaining 89 from institutions, mainly Universities and Colleges (40), Commonwealth and State Govern- ment Departments (30), private firms (9), museums (5), and sundry research institutions (5). A total of 2211 items were received and processed from 375 institutions, mainly through exchange of the Journal and Proceedings. Council expresses great gratitude to Mr. J.L. Griffith, the Honorary Librarian, and to Mrs. Grace Proctor, the Honorary Assistant Librarian, for all of their work during the year. Because of the imminent sale of the Science Centre building, Council resolved, at its meeting on 30th March, 1983, that the library books and shelving be moved from the space presently occupied by 3lst May, 1983 or as soon thereafter as possible, and that accessioning of serials and provision of service in photocopying and facilities for readers cease on Thursday 28th April, 1983. AWARDS The following awards for 1982 were made: Clarke Medal: Emeritus Professor Noel Charles William Beadle Edgeworth David Medal: Nhan Phan-Thien The Society Medal: William Broderick Smith- White Liversidge Research Lectureship: Graig: Professor D.P. SUMMER SCHOOL A most successful Summer School in Engineering was held at the University of Sydney from 24th to 28th January, 1983. 80 students, who had completed Year 11, attended the School. The School covered a wide range of engineering topics, and included visits to I.C.I., Qantas, Pyromont Power Station, Railways Signalling and Control,Telecom Exchange, and MWS and DB Treatment Works, North Head. FINANCE The audited Annual Accounts accompanying this report show that the Society's normal funds are in as good a state as can be expected in these difficult times and that the operations in 1982 resulted in a deficit of $614. The deficit result- ed almost entirely from the reduction in the N.S.W. Government grant from $1600 in 1981 to $1000 in the year of the account. Fortunately it was possible to balance unavoidable rises in the cost of some items by increased revenue from investments. Unfortunately the overall outlook for the bulk of the Society's total assets of about $520,000 is not bright. You will note that the Auditor has qualified the Accounts, pointing out that there is a very substantial deficiency of shareholders' funds in the Society's joint venture with the Linnean Society of N.S.W. - "Science House Pty. Ltd.!' In the light of the Auditor's report we must very regretfully prepare ourselves for the possibility that over $400,000 of the Society's assets, lent as an unsecured loan to Science House Pty. Ltd., may not be recoverable in part or whole. The year 1983 should see a resolution of the uncertainties over this matter. Some members of your Council, including the Honorary Treasurer, have not regarded as realistic the continuing optimism amongst the supporters of Science House Pty. Ltd. that it will be able to resolve its difficulties and survive; the interst burden ($2M) on the original mortgage loan ($1.5M) has become too large ever to reduce by trading alone, and a sale of the Science Centre building appears inevitable. Financial planning for the Society in 1983 has thus to allow for the contingency that substantial relocation expenses may be incurred if the Society is forced to move its office and possessions. Council is grateful to the New South Wales Government for its grant through the Division of Cultural Activities in the Premier's Department. 42 ANNUAL REPORT OF COUNCIL SCIENGE CENTRE Council's representatives on the Board of Science House Pty. Ltd. continued to be Mr. M.J. Puttock (Chairman), Mr. E.K. Chaffer, Mr. J. W. Humphries and Associate Professor W.E. Smith. They gave considerable attention to the financial difficulties of the Company and warned Council that in 1983 substantial changes in arrangements would probably be necessary. The Science House Pty. Ltd. Secretariat serviced 21 scientific societies during the year - a benefit which they greatly appreciated. ACKNOWLEDGEMENTS Mrs. Judith Day and Mrs. Grace Proctor in the past year have continued to give great assitance and service to the Society and its members. Council would also like to record its thanks to all those who contributed to the success of the Summer School in Engineering, especially to Professor T.W. Cole, of the School of Electrical Engineering who organized the Summer School. FINANCIAL STATEMENTS For the year ended 31st December, 1982 AUDITORS REPORT The Society advanced an amount of $416995 to Science House Pty Limited in 1974 (refer note 3) which amount appears in the Balance Sheet as an"Unsecured Loan to an Associated Corporation” The accounts of Science House Pty Limited, as at 30th June 1982, show a deficiency in shareholders funds of $708170. We have been unable to confirm that a material improvement in this situation has emerged prior to the date of this report and accordingly we are of the opinion that some or all of the loan money may not be recoverable. No provision for the non-recoverability of this loan has been made in the accounts of the Society. Subject to the above, in our opinion: (a) the attached Balance Sheet and Income and Expenditure Account, which have been prepared under the historical costs convention, are properly drawn up in accordance with the Rules of the Society and so as to give a true and fair view of the state of affairs of the Society at 31st December 1982 and of the results of the Society for the year ended on that date: and (b) the accounting records and other records, and the registers required by the Rules to be kept by the Society have been properly kept in accordance with the provisions of those Rules. WYLIE & PUTTOCK Chartered Accountants. By ALAN M. PUTTOCK Registered under the Public Accountants Registration Act, 1945 as amended, 43 FINANCIAL STATEMENTS ST*° 20662 eS ¥8OSZ 00°0OS 00°000S S9°1T8e co’ rt LS*vbl TO°ELEbZS 00° O00T 00°0O S9°18e dea, yueting SGNNd GaLWINWNIIY (pb 930uU) Tejytdej puny ysenbag eBpIstaaty] 0}F Aezsuesr (CP)T 970U) Setzrp~Toey Azeaqiy jO UOTSTAOIg JOJ ZUSWUkeY puny AteIqIy 0} Aazsuesay NOILWIYdONddY YOd ATAVTIVAY JeaR jo Hhutuuthag - spunj pezer[nunsoy pund AieIqt] worlj Jazsuerl jJaopusebbog ‘*3'm a3e7] 93e45S9 Spsad0ig puny Aterzqty 0} 4YSeTAaUT Y SUOTReUDG aeak 3JoJ LIDIAgIA 7861 Aequecseq 4ySTE papug AeaA ay 30Y 19° beeely 0o*T Ce SQGNNd GaLVINKNDOY 43JO LNAWALWLS Jeianseary ATeTOUOH AYG ‘WW quaptseig 3109 ‘A'L SLASSW LAN uOT}IOq JUSTIND-UON - suotjydtazosqns Silsquay ajtq SHILITIGWI1 LNAYYND-NON +8597 peinsesuy - sueoy] 3 saouPApY 3509 3e - saazeys 930U) SNOILVYOdYOD GaLWIDOSSW - PPV ere ane? 00° O0ZLEs 9E°ZSPOT 00° 00°0005 ee Oe eg 99° 09161 9E°2SPS 88° 9558 6S°8S2bZ 08° 60S 00°0 bL°91S1 gtemcy ce leases eee L¥°968Z (EL 9ZZ) 121 Y6 85° 6S61S SSS SSS es ve°e9T AAR 0S°O2S8Z 65° 99E8T ZS C1L 61S 82° 6E0E 19° S666 18 50° testy 19° P666IP ee 00°! 00°O00ST 00°00009 00°00Z28 OO°O09ET 99°0SSS LZ°STIt oo°es Ze 61 €€° 8029 8S°6Z0T 19° E1T0S 96° T62E 00°0 69° LOC? CIVLOC 90°82 CB/CT/TE S}tsodeq Hbhutszeag 4sataquy] a6e6310W uo sueo7q Y90RS peqtazosu] 3 Spuog YT eamuoWWO) SLNAUWLSAANI :ppy uoTzeTIe1daq SS89T 3#SOD ye - saianzotd UOTRFENTEA 9E6T - AACIAQTT uot}etoaideq ssat ysoo ze -"'939 ‘Qusaudtnby ®9TJJO ‘9anqztuang SLAUSSW GdaXI4d : PPV SLASSW LINAX¥YND LIAN @OUPAPY UT pTed Teurinor 03 suotydtazoqns @ouePApPY UT pled suotydtazosqns dtysirsequay uOT}10d quezing - suotydtaosqns STsquay ast] sTenazs9y 8 S10}Tpeazj AaApuns SSILITIGWVIT LNaYYdND + sse7 yueg ze yseo) qytsodeq Hbutiaesg ysataju] s}yuswkedseig 3 8103q9q 19430 §399qd [Nj 3qGnN0qG JOjJ UOTSTAOIdg sSaq suo t3ydtazosqns 10} s1i0j4qeq ysoadwy yse) Aj 3eq SL3SSW LNaYdND :A4q pajueseiday SQNN4 GNW SHAYXaSAY TWLOL SGNNd GaLWINWNIDY (py @30U) SGNN4d LSnuL ((9)2 pure (P)(2)T S$8}0U) GNNd AYVUGIT ((4)2 a}OU) aATeSaeYy UOTAdUNsSay ((Pe)2 a}ou) aeAteasay ATeIAqT) SaAddSaY ze se LAAHS JONWIVG SATY¥M HLNOS MAN dO ALAIDOS IWAOUN FHL 00° O0T8Z 00°0000S 00°00002 00°0018 16°ZLE912 00°O09ET 99-8209 S@° Peel p8°S96 vb v6 Leet bL°212S v9°LEZ8 96°0&29 00°0O vO° 2261 OS*6rOT OS*6rOl b9°e?e 2S" P8OSZ 9€°SSPLI EL 8022 00° 1669TP LS*O1EL FINANCIAL STATEMENTS 44 19° V6661P 19° POOE Spunj pazertnunsoy 00° O0669TP @ATesaz uotydunsay Hutqusesaiday 19° V666I1P Jequeseq ys TE Re soUeTeYG 19° V6661P Azenuer Ys], je soueyleg "ESET ‘Tequacseq ystE 03 AOotTad pazedtotqzue are squawAedat Tetzaqjew ON “‘TTeI We eTqeAedar stseq aatj 4SazeajuT ue uo useq aaey suedwod ayy 0} SueOT pue saouPApY “qysozaequt %9G e sey AZaTIOS Yoeea yotym UT paewzojJ usaq sey ‘paqztwty Ayd esNnoYH |asouaTIS ‘Aueduoa eB “STYQR SPERTTIOeJF OL*SuOtynAIyYSsut IJtwapeose pue ItjJTyUSTIS “Teuotsseajoid JOJ SATJITIIEJF aptaoid 03 SSTemM YINOS MAN JAOJ @tjusy asdUuEeTIS e& JO UOTJeTedO pue JUSsWYsTTqeq4ss syy AozJ AZaTIOS URBUUTT 84 YRTM SAINqUeA AUTOL e& OUT paaTaqua sey ARaTIOS ay] NOILWYOduYOD GaALVIOOSSY OL NWO1'E 82° 6E0€ se* vol spunj [Tezrauah of Hbutamg 00°0062 Y9O}S paqtazosut pue spuog YR, eenuouwo) el’ bre yueg ze yseg :Aq pazussaidsay 82° 6E0E Jaequacseq 3STE ye adueTeg 00°0S 00°0O S9TJITTIeJ ATeIqI, a1 pled 00°0Os seseyoind Arzeazqriy] ssa 82° 680€ S9° TBE ysatequt yueq pue suot}euog ppy EL’ 8022 Ajenuer 4s] ze souepeg pung Areiqty (9) 19° vOO0E 00° O669TF 19° V666TP Se bs 00° O02 8 CoP 00°000S O08 6h €6°LS22 9E°?SPS LS°SO0E2 (2U09) SHAYSSIY GNV SNOISIAOUd NI SLNANSAON 00°O669lF oo'T LS°OTEL uotTzezr0d109 00°O669lF pazeloossy 0} ueoq uotjejrodioyj OO’! pezetsossy ut sarzeys :Aq pejueseideay Jequeseqd YSTE ze souePTeg 00° 1l669TF Azenuer 4ST ze eoueyeg 00°16691b eAtTesay uotqydwunssy (q) dequeced 3si¢ ye aaueTea ZS"OIEL Azenuer 3S] je aoueyeg yecgven |) eAteasay ATeIqT] (2) SAAMNS3SAY ANY SNOISIAONd NI SLNANSAOW °2 ‘asodind 3ey, toj Bbuteq se zouop ayy Aq pajzeubtsep ATTedtjJtaeds suotyeuop yusseideaIr sqzuewded yong *AjatTIOS 9Yyy JOJ SaTAQITTIeZ AATeAGT]T Hutptaoad jo 3509 984} SpreMOR (Ff |B}JOU OSTeS 9asS) PpaxtTwty A¥q BSNOH aduaTIS 0} pred useq aaey puny AAeIqty] §s,A}9TSOS ayy OF SUOTJeUOP UTeRIIaD Sat zITToey Areaqty (P) ‘azeak YUueTINSD 9yy ut paydope you sen einpesso0id styl *‘AATeIqT] BYR JOJF paatnbdoe are satyatao0s Aay RO Jo suotzeot{tqnd ayy Aqeszaym suwerbord ebueyoxse ayy ut pasaAToAut sHhutpsso0rIg 3 TeUuINOLG ayy JO satdods asoyy HhuttTtew ¥ Hutqzutad JO 3809 ay} OF UOTANGTI}UOD e& Se Spuny pazetNunddsy Of puny AJeIGtIy ey} WOT parTTazysuezzZ sem JZUNOWe Ue APSA QRET AYR Hutang puny Arerzqty (3) %00°ST quaudtnby e5TF30 %0S°L eanzTuand :97e asn ut saqzer Tenuue Tedtoutiad ayL *szeak Jaze, ut s3soo Atedser paqzedtotque AOjJ MOTTE OR se oS STSeq SNTRA UMOP USRZAITIM e UO Pa RPeTNITeI ST uoTzPetIeIdaq uotzetoeideq (q) S$js09 TeITAOYSTY JO Stseq ayy uo parzedaiad useq saeYy sjZUNOdIe syL Hutjzunoooy jo stseg (e&) azeak Butpasaid ayy ut paqdope oste etzem sataotytod Hbutqjunoosse yons ‘peqzeqs aestmiseyuzO ssatuNn ‘"Z86] ‘Aequaseq ys{E pepus Aeaetk sy JojJ sj}unosoe szt jo uotzeredaad ayRz ut AZatIOS sy Aq paqdope S9TITTOd HutTjunos.e YUeSTJTUHTIS Syy sre TJapunstay yno yas SHIDITOd ONILNNODOW LNYOIAINDSIS dO AYYWHNS “1 2861 Jequeceq 4STE SLNMODOV 3HL dO Luvd pepug tea, ayy 304 SNIWYOd ANY OL SALON FINANCIAL STATEMENTS 19° 0f6 00°O L£L° 2002 00°009S Le" 6t (Ol LZS21) o00°o00s 00°0O OO*hS6T S9°T8e 00°O 61° 2672S 2L' Spel oo°Ee7s cO° VTS 00°O spunj HbutyIrOmM ut esearsu] BaTPITToOez ATeIqry sesuedxa punj ysniy SJuUsUyYsSsAUT UT aseaITDU] aaueape ut suotqydtszosqns sirsequew OFTT JO UOT PROTFTISSeTIIY suoTIeIedoO 0} peat{tdde spung s3qep INjqzqnop AOF uoTtstaAoijd Szoesse PexTJ JO uoTtxyetdaidagq ;potted yuetTino ayy ut spunj jo AeTINO ay HutaTOAUT You sway :sso] azeask ayy JOJ YIDTJep Hhutyeszadg SQNN4d dO NOILWOITIddv¥ jJatopusebhhog ‘J'm e3ey aqeqsg speas0ig 93e45q eTTO - S}senbeq punj ysniy ewoout punjJ 4snIiy punj Azeaqtyt o3 ZSaTaqzUT pue suoTtzeu0g suotjzejzedo WOT} PeATIep spuny s3qep InNjqyqnop AOZ uotstaojg sjaesse PeXTJ JO uot }etIaId9aq :pottzed Juetzind 9sy}z ut spunj jo AeT NO ayy HutaToauTt you suaqy] > PPW azeak ayy Joj sn{dins Sutzeszsdg SQNNd JO FouNOS 27861 Jequeseq 4S1¢ papug Jee, ayy I0¥ SGNN4 4O NOILWOIIdd¥ GNY 39UNOS dO LNAWALVIS 00°O 6l'c6cl vp S66 SL°962 S2° be? 0o°12s spund 4sna] Teo] Jequecseq 4STE ze asoueTeg uOoTJeSTTeRIdeD ssaq Azenuer 4S] ze aoueyeg potted JOjJ ainytpuedxg ssaqy POTI8q AOZ BwODUT anuaaay enusasy —- puny ysenbeg aT To OO LEvE 00° 000s 00°269 00°02Sz 00'6T 00°O 00°19bZ OO 6ZbT oo 2sbs 00°9L22 00°126 00°62S 00°92z2 S6°8E2 6€°ve?zt cL 99€ cL’ 99€ 00°O00F vS"OOTE vS* Oot 00°o00€ Le°b29N L2°e79t 00° o00€e 6S°6VES 6S°6PE 00°000s Jaquecseq 4ysTE ze |aoueTeg 00°0 anusaay pazerTnwunssy jo uotzestyleqztdeg 00°0 peatasey yTeqtIde) ysanbag 00°000F Azenuer 4s] ye aouejyeg yezytdej - puny ysenbeg ato Jaqueseq 4YseTE je aoueTeg 19° ESL Azenuee 4s] ye aouejyeg COTES) Ol’ vce potted JO} ainjitpuedxy sseq OO’ I6E POTIaq JOJF |wodUT anuansay anusaay - puny ysenbeg ebptsiraaty Jaquasaq 4yS1E ye soUeTeG 00°OOo0t spuny pazyertnunooy WOlj Jojsuesl 00°000z Arenuer Ys] 3e aouerzeg Teqytdej - puny ysaenbag abptsszaaty Jaquacseaq 4STE }e eoduPTeg Le°ee?er Azenuer 4S] 3e aeouereg OO°16€ 00°0 potiad JOjJ sinzyIpuedxg ssaq OO°T6E PpoOtiaq TOF B9wOdUT snNUsAdY anuaney - puny aZTJg 44TJING 39a4TeCM Jaquacseq 4ySTE 3e adueTeg 00‘O000€ Aqenuer 4s] ze aouerteg Teztdeg - pung eztad 331j4Ng 1931 eM Jaquacseq 4ysTE ze aoueTeg 00° 002 uoTzestTTezyide) ssaq 6S°69S TO°e€rel Ajenuer 4ST 3e soueTeG (2b ° £69) Ch VPEel potidad JOJ ainjzIpuedxgZ ssa] oo°rs9 POTI9d JOF SwOdUT snusaAdy anuaAsy - puny TeTtToOwWaW ayrel[D Jaqueseq 4ysTE ze aduerTeg 00002 anusaesy pazernunsoy jo uoTzesTTeqyIdeg 00°008F Arenuer YsT je asoueyt eg TejytIdep) - puny Tetroway ayszeTID SGNNd LSNYL “Fb 00°O00Fr 00"6E2 00°19P2 oo" o0et v9" E8TZ (9T°ET) 08° 961 00" Lee 00° 0002 00°0002 Leelee OS‘ 8ZO0l LL° Pst €2° 981 OO’ TPE 00°o00€e 00° o000€ 10°€bro9 00°0 92°02 vl’ ¥dy 0o0°StS 00°O08r 00° O08F FINANCIAL STATEMENTS 46 cO°COET? 69° 981 LQTETE EE" Le 00°S2 00°9 OL°98E€ 91° 2288 LV°S8PIT 00° o00t OZL°190€ LL SCV 02° 6SeZ v8" Oce auoydeTelL Tv 6PTS SeTrzeyTtes 00°0 ates uo ssoqy —- squtadey 00°0 aoueuaqUTeR yY SsAteday p2° 1822 quseY cl’ Shel s3q9d Inj3zqnoqg JoJ uotstAojid 08°89P yTe4r9sue5 - AZauotzeyYS BY Hutyutagd 86° 082 a6He sod LESENEL uot4yngt3z34siqg § Hutqutrd 3Ja}VaTSMAN C2° PP sasuedxg Hutzoan ATYRUOW 68°62 sesuedxg snoauel[[a0sTH 99° EEF aoueinsuy Areazqty OO'TET SadTAIaS Japeay 3 HbutnboTezeg “uotsseaay AreIqqty 00°OS saseyoing AreIqty €6°999S O° coor afejysog 3 butddei4m €8°v99b aUNTOA Jeax YUuerAnD - Hutqutag S480) uotz}eoT{[qnd [eudnoc 16°202 aoueinsu] ST’ PZe seasuedxqg JUswUTeIaUA SS°09¥F Jamodg & 3YHT] 9143z9eTF oo°e7s uoTyeroeideg 00°92T butueata 00°OST A}ZeTIOG ayy JO sayduejg 00°99F saej JIpny 00°?2E6 seaq Aduequnoooy SASNddXga-S597 awoouy 329ayAO sn{ding ~Tooyos iaewwns sn{tdang Jauutqg Tenuuy suotzeot{[Tqnd T9430 JO 9TeS slequnn yoeg jo ayes sqzutidey jo ates Peatadcsay 4ysataqu] awoosuy ~Teurnogr pue dtyszequeyq Te OL Aptsqnsg juawuraAoy Teuanor oj} suotydtazosqns seaq uotzeottddy Slequay ajytqT - suotjdtazosqns dtysisaquey Azeutpjo - suotqjdtaosqns dtysraquey JWHOONI 2861 Jequeseq 4ySTE pepug AweeA ayy Jog LNMODDY 3YMLIGN3dXa ANY SWOONI vL° L272 LO'€8Ze OL’ ere OL°96T b2° 1822 00°126 vS° TSP 8S°692 L£e°eS2t SO°€9S 8E 622 pL°S2pb 0O0°Szt 08° 6¥ S8°691S S8°ZEOl OO*2ETP 98° LL1 S2*O0ce 0c °9S€ 00°62S 0s* S02 00°O0T OO°ebe 00°298 09°S6S0z2 11° 282 Sl°62 b6°S7¢ 09°Ss 00°OSEe 00°0O ST°86S2 S9°PS22I 00°0091 BE LCTE LEG L2SL OS*OShL ANNUAL REPORT OF COUNCIL ABSTRACT OF PROCEEDINGS 1982 - 1983 The Annual General Meeting and eight General Monthly Meetings were held in the Science Centre. Abstracts of the proceedings ot these meetings are given below. In addition the Liversidge Research Lecture was deliver on 20th May, 1982 by Professor D.P. Craig. APRIL 7th 115th Annual General Meeting. Location: the Auditorium, lst Floor, Science Centre. The President, Professor B.A. Warren, was in the Chair and 35 members and visitors were present. The Annual Report of Council and the Annual Statement of Accounts were adopted. 3 papers were read by title only. The Clarke Medal was awarded to Professor William Stephenson; the Edgeworth David Medal to Dr. Martin Andrew Green; the Society Medal to Associate Professor William Eric Smith and the Olle Prize to Dr. Helene Martin. Messrs. Wylie and Puttock, Chartered Account- ants, were elected Auditor. The Presidential Address ''Understanding the Cancer Process: How the Study of the Secondary Deposit Helps'' was delivered by Professor Warren. The incoming President, Professor T.W. Cole, was installed and introduced to members. MAY 5th 939th General Monthly Meeting. Location: Auditorium, 1st Floor, Science Centre. The President, Professor T.W. Cole, was in the Chair and 29 members and visitors were present. 1 new member was elected. A symposium was held with the theme "Development of the Hunter Valley". The panel of speakers eomprised Mr. R.H. Read, Officer-in- Charge, Parramatta Branch, N.S.W. Department of Agriculture; Mr. K. Grezl, Research and Development Officer, Hunter Development Board, Newcastle; and Mr. R. Rollinson, Engineer, Projects Planning, Electricity Commission of N.S.W. JUNE 2nd 940th General Monthly Meeting. Location: Room H, 2nd Floor, Science Centre. The President, Professor T.W. Cole, was in the Chair, and 17 members and visitors were present. An address entitled "Electricity Production Using Silicon Solar Cells" was delivered by Dr. Martin Green of the School of Electrical Engineer- ing and Computer Science, University of N.S.W. JULY 7th 941st General Monthly Meeting. Location: Room E, 2nd Floor, Science Centre. The President, Professor T.W. Cole, was in the Chair, and 22 members and visitors were present. 1 paper was read by title only. 1 new member was elected. 47 An address entitled ''Palynology - the Study of Spores and Pollen'' was delivered by Dr. H.A. Martin of the School of Botany, University of N.S.W. AUGUST 4th 942nd General Monthly Meeting. Location: Room H, 2nd Floor, Science Centre. The President, Professor T.W. Cole, was in the Chair, and 21 members and visitors were present. 3 new members were elected. 1 paper was read by title only. An address entitled "Higher Education - Only Change is Constant" was delivered by Mr. R.E. Parry, Chairman, N.S.W. Higher Education Board. SEPTEMBER 1st 943rd General Monthly Meeting. Location: Room H, 2nd Floor, Science Centre. The President, Professor T.W. Cole, was in the Chair, and 17 members and visitors were present. 4 new members were elected. An address entitled 'Development of Metal Technology and the Use of Metals in Traditional Australian Buildings' was delivered by Associate Professor M. Hatherly of the School of Metallurgy, University of N.S.W. OCTOBER 6th 944th General Monthly Meeting. Location: the Auditorium, 1st Floor, Science Centre. The President, Professor T.W. Cole, was in the Chair, and 19 members and visitors were present. 1 new member was elected. An address entitled "What is a Teaching Hospital?" was delivered by Professor J.B. Hickie, AO, Professor of Medicine, University of N.S.W. and St. Vincent's Hospital. NOVEMBER 3rd 945th General Monthly Meeting. Location: Room H, 2nd Floor, Science Centre. The President, Professor T.W. Cole, was in the Chair, and 30 members and visitors were present. 1 new member was elected. 2 papers were read by title only. An address entitled "'How to Avoid a Migraine Headache" was delivered by Professor M. Anthony, Neurologist at Prince Henry Hospital. DECEMBER lst 946th General Monthly Meeting. Location: Room E, 2nd Floor, Science Centre. The President, Professor T.W. Cole, was in the Chair, and 27 members and visitors were present. 1 new member was elected. An address entitled "Computer Graphics" was delivered by Dr. D. Herbison-Evans of the Basser Department of Computer Science, University of Sydney. 48 ANNUAL REPORT OF COUNCIL CITATIONS THE CLARKE MEDAL The Clarke Medal for 1982 is awarded to Noel Charles William Beadle, D.Sc. (Syd.), Emeritus Professor of Botany of the University of New England. Professor Beadle has played an outstanding role in the development of Australian botany over the past 40 years. Firstly, he produced the first authoritative account of the vegetation of western New South Wales (Beadle, N.C.W., 1948: The Vegetatton and Pastures of Western New South Wales. Sydney: NSW Government Printer). He carried out this work while he was Research Officer and Botanist with the N.S.W. Soil Conservation Service, and the work was embodied in a thesis for which the University of Sydney awarded him the degree of D.Sc. Secondly, he demonstrated the close relationship many plant communities in Australia show to soil phosphate status in their distributions. Thirdly, as a university teacher concerned that undergraduates should be readily able to identify plants, he has been actively involved in the production of regional floras. The first of these is the Handbook of the Vascular Plants of the Sydney District and Blue Mountains. This was published in 1963 and arose from his time in the University of Sydney as a lecturer and senior lecturer. This handbook is the direct forerunner of the recently published third edition of Beadle, N.C.W., Evans, 0.D. and Carolin, R.C. (1982): Flora of the Sydney Regton. The second, Students’ Flora of North Eastern New South Wales, a flora in six parts, of which four have been completed, arose following his appointment in 1954 as foundation Professor of Botany in the University of New England. Lastly, he is author of a volume which will be for many years to come, the definite work on the vegetation of Australia (Beadle, N.C.W. (1981): The Vegetatton of Australia. Cambridge: Cambridge University Press). Noel Beadle has inspired generations of students with the breadth and enthusiasm of his approach and his books and many papers have become standard references for professional plant ecologists and tor other scientists and persons interested in the Australian vegetation, its distribution, dynamics and history. It is fitting that he should be honoured for outstanding work, which has continued up to the present time, towards the understanding of the vegetation and flora of this continent. EDGEWORTH DAVID MEDAL Dr. Nhan Phan-Thien is awarded the Edgeworth David Medal for 1982 for his outstanding work in the field of mechanics. Dr. Phan-Thien is a lecturer in the Department of Mechanical Engineering of the University of Sydney. He graduated from Sydney University in 1975 with First Class Honours, the University Medal and the Charles Kolling Prize, after studying under a Columbo Plan Scholarship. He gained his Ph.D. in 1978 with a thesis entitled "Some Constitutive Equations for Dilute and Concentrated Polymeric Liquids". He is quite clearly the outstanding young person in the area of mechanics in Australia today. He is astonishingly productive and lives and breathes research, producing 64 papers since 1977, a rate about ten times the norm. The diversity of the research problems treated is very striking, ranging from fluid mechanics to solid mechanics. Dr. Phan-Thien is a very worthy recipient of the Edgeworth David Medal for 1982. THE SOCIETY'S MEDAL The Society's Medal for contributions to the progress of the Society and to science is awarded to William Broderick Smith-White, M.A. (Cambridge), B.Sc. (Sydney). Associate Professor Smith-White joined the Royal Society of New South Wales in 1947. He served on Council for a total of ten years, being first elected in 1960, becoming President in 1962 and Vice-Presid- ent in 1963 and 1964. He rejoined the Council in 1971 and served until 1976. In this later period he carried through a complex calculation of the compounded membership fees necessary for a range of ages and length of previous membership. He contributed four papers to the Society's Journal, including his Presidential Address entitled ''The Mathematical Sciences in the Changing World". Bill Smith-White gained his Bachelor of Science from the University of Sydney with first class honours in both mathematics and physics in 1930. He was awarded the Barker Graduate Travelling Scholar- ANNUAL REPORT OF COUNCIL 49 CITATIONS ship in mathematics and proceeded to Cambridge University, where he achieved a Bachelor of Arts after two years' study. Returning to Australia he accepted Professor Wellish's invitation to join the Mathematics Department of Sydney University where he was appointed Acting Lecturer in 1933 and 1934. He was subsequently a Tutor at Melbourne University for two years and returned to Sydney in 1937. There he progressed through various grades, being Senior Lecturer in the 1950's, until in 1960 he was promoted Associate Professor in the specialist field of Analysis. He retired in 1974. His brother, Spencer Smith-White, the plant geneticist, was also at Sydney University for many years. Bill Smith-White is fondly remembered by his many students for his clear, systematic lectures and pleasant personality. He is also warmly regarded in our Society, and the Council is delighted that he has agreed to accept the Society's Medal. 50 OBITUARY DANIEL JOSEPH KELLY O'CONNELL, S.J. On 14th October, 1982 at the headquarters of the Jesuit order in Rome, Daniel J.K. O'Connell died peacefully at the age of 86. Fr. O'Connell was elected a member of the Royal Society of N.S.W. in 1935 and published three papers in the Journal and Proceedings. He served on Council from 1946 to 1949 and was a Vice-President from 1950 to 1952. In 1953 he became an honorary member. Fr. O'Connell was born at Rugby in England on 25th July, 1896, He was educated at Clongowes Wood College in Ireland and joined the Jesuit Order on 8th September, 1913. In 1920 he completed his M.Sc. at the National University of Ireland and was awarded a travelling studentship in mathematics. Arrange- ments were made for him to enter the University of Cambridge, However, on account of poor health, after completion of his philosophical studies at Valkenburg, in Holland, in 1922, he arrived in Sydney to be- come Physics Master and Second Division Prefect at St, Ignatius College, Riverview. In 1926, he returned to Dublin to study theology and he was ordained a Jesuit priest on 3lst July, 1928. He completed a final year of pastoral theology study from mid-1930 to mid-1931 and then for two years worked at Harvard College Observatory under Professor Harlow Shapley. He completed his Ph.D, studies and returned to Riverview via Mount Wilson and Lick observatories, Japan, China, the Philippines and Java, arriving in December, 1933. Fr. O'Connell became Director of Riverview College Observatory on lst January, 1938. The three papers he published in the Journal and Proceedings of the Royal Society of N.S.W, were about earthquakes and the Galitzin seismograph. However, Fr. O'Connell's main area of study was the variation of light from double stars that re- volve round one another and eclipse each other twice each revolution to observers here on earth, These variable stars were observed from Riverview on clear nights and a difficulty arose in constructing a curve of the variation of light with time if the orbit of the lighter star relative to the heavier one was ro- tating (rotation of apsides). If we are looking along the major axis of the elliptical orbit, the eclipse of the fainter star comes exactly half a period after the eclipse of the brighter star. If, however, we are looking along the line at right angles to the major axis of the orbit, the interval between eclipses will be shorter when the lighter star is nearer the heavier star (periastron) than when it is further from the heavier star. When rotation of apsides occurred, the position of the eclipse of the fainter star by the brighter star moved on the curve of the variation of light with time relative to the position of the eclipse of the brighter star by the fainter star. Fr. O'Connell studied many eclipsing double stars whose orbits showed rotating apsides, but the O'Connell effect, named after him, is distinct from rotation of apsides. It is that the light maximum following the eclipse of the brighter star is brighter than the light maximum following the eclipse of the fainter star in many eclipsing double stars. Fr. O'Connell considered what he called ''the so-called periastron effect in close eclipsing binaries" in a publication of Riverview College Observatory in 1951. It had been suggested in 1906 that a tidal effect occurred between double stars at periastron and, as a result, their radiation increased, However, in 1916, a pair of stars were observed to brighten when they were not at periastron. Fr. O'Connell favoured the explanation that close double stars are embedded in a rotating stream of gas and the stream of gas from the brighter to the fainter star is hotter and brighter than the stream from the fainter to the brighter star, After the eclipse of the brighter star we see the stream of gas from the brighter to the fainter star (in addition to the two stars), whereas, after the eclipse of the fainter star, we see the cooler, darker stream of gas from the fainter to the brighter star. In 1949, Fr. O'Connell received a D.Sc. from the National University of Ireland. On 26th July, 1952, having just turned 56 years of age, he left Riverview College Observatory to become Director of the Vatican Observatory. Vatican Observatory is at Castel Gandolfo, the Pope's summer residence, on the western side of Lake Albano, 26 km south of Rome. In 1952, the International Astronomical Union met in Rome and Pope Pius XII gave an audience and reception for the astronomers. Later, under Pope Pius XII, the major modern research tool of the Vatican Observatory, the 63/98/240 cm Schmidt telescope, was com- pleted and inaugurated; Fr. O'Connell published a report on this instrument in 1955. From 1955 to 1961, he was President of the Commission on Double Stars of the International Astronomical Union. In 1957, Fr. O'Connell organized a Study Week of the Pontifical Academy of Sciences on Stellar Populations. Pope Pius XII addressed the conference (Fig. 1) and many of the world's most capable astronomers attended it (Figs. 2 and 3). Fr. O'Connell edited the proceedings of the conference in 1958. Also, in 1958, he published "The Green Flash", an account of the thin green slit of light sometimes seen for a fraction of a second at the upper edge of the setting or rising sun. In 1970, Fr. O'Connell organi- zed a second Study Week of the Pontifical Academy of Sciences on the Muclet of Galaxies, and he edited OBITUARY >i the proceedings of the conference in 1971. Fr. O'Connell retired as Director of the Vatican Observatory in 1970. He was President of the Pontifical Academy of Sciences from 1968 to 1972. Although he worked very hard, he always had time to talk with friends. He is remembered at St. Ignatius College, Riverview, for showing groups of boys the moon, planets and stars on clear nights and for his unfailing gracious word and cheery smile for staff and boys alike. Fr. O'Connell was very intelligent, hard working and always a gentleman. Eg sl. Pope Pius XII and Fr. O'Connell after the Pope's address to the astronomers at the Pontifical Academy of Sciences, 20 May, 1957 (taken by Abbe Georges Lemaitre) . Fig, 2. Pr. O'Connell and Professor Fred Hoyle at the Catacombs of St. Callistus, 23 May 1957 (taken. by Abbe Georges Lemaitre). 52 OBITUARY Fig. 3. Fr. O'Connell with Professor and Mrs. J.H. Oort at Grottaferrata, 23 May: ~1957.. “ “ip Y YYW, Y Lo Wj. Lawrence A. Drake, S.J. NOTICE TO AUTHORS A “Style Guide to Authors” is available from the Honorary Secretary, Royal Society of New South Wales, PO Box N112, Grosvenor Street, NSW 2000, and intending authors must read the guide before preparing their manu- script for review. The more important requirements are summarized below. GENERAL Manuscripts should be addressed to the Honorary Secretary (address given above). Manuscripts submitted by a non-member must be com- municated by a member of the Society. Each manuscript will be scrutinised by the Publications Committee before being sent to an independent referee who will advise the Council of the Society on the acceptability of the paper. In the event of rejection, manuscripts may be sent to two other referees. Papers, other than those specially invited by Council, will only be considered if the content is substantially new material which has not been published previously, has not been submitted concurrently elsewhere, nor is likely to be published substantially in the same form elsewhere. Well- known work and experimental procedure should be referred to only briefly, and extensive reviews and historical surveys should, as a rule, be avoided. Letters to the Editor and short notes may also be submitted for publication. Original papers or illustrations published in the Journal and Proceedings of the Society may be reproduced only with the permission of the author and of the Council of the Society; the usual acknowledgements must be made. Offset printing with “Typeset-it-Y ourself” preparation of a master manuscript suitable for photography is used in the production of the Journal. Authors will be supplied with a set of special format paper. An IBM Selectric (Golf Ball) typewriter with ADJUTANT 12 typeface must be used. Bio- logical and reference material are shown in Light Italic. Symbol |2 has most type required for mathematical expres- sions and formulae. Detailed instructions for the typist are included in the Style Guide. PRESENTATION OF INITIAL MANUSCRIPT FOR REVIEW Typescripts should be submitted on heavy bond A4 paper. A second copy of both text and illustrations is required for office use. This may bea clear carbon or photographic copy. Manuscripts, including the abstract, captions for illus- trations and tables, acknowledgments and references should be typed in double spacing on one side of the paper only. Manuscripts should be arranged in the following order: title; name(s) of author(s); abstract; introduction; main text; conclusions and/or summary; acknowledgments; refer- ences; appendices; name of Institution/ Organisation where work carried out/or private address as applicable; date manuscript received by the Society. A table of contents va also accompany the paper for the guidance of the ditor. Spelling follows “The Concise Oxford Dictionary”. The Systeme International d’Unites (SI) is to be used, with the abbreviations and symbols set out in Australian Standard AS1000. All stratigraphic names must conform with the Inter- national Stratigraphic Guide and must first be cleared with the Central Register of Australian Stratigraphic Names, Bureau of Mineral Resources, Geology and Geophysics, Canberra. The letter of approval should be submitted with the manuscript. Abstract. A brief but fully informative abstract must be provided. Tables should be adjusted for size to fit the format paper of the final publication. Units of measurement should always be indicated in the headings of the columns or rows to which they apply. Tables should be numbered (serially) with Arabic numerals and must have a caption. Illustrations. When submitting a paper for review all illus- trations should be in the form and size intended for insertion in the master manuscript. If this is not readily possible then an indication of the required reduction (such as reduce to '4 size) must be clearly stated. Note: There is a reduction of 30% from the master manu- script to the printed page in the journal. Maps, diagrams and graphs should generally not be larger than a single page. However, larger figures can be printed across two opposite pages. Drawings should be made in black Indian ink on white drawing paper, tracing cloth or light-blue lined graph paper. All lines and hatching or stripping should be even and sufficiently thick to allow appropriate reduction without loss of detail. The scale of maps or diagrams must be given in bar form. Half-tone illustrations (photographs) should be included only when essential and should be presented on glossy paper (no negative is required). Diagrams, graphs, maps and photographs must be numbered consecutively with Arabic numerals in a single sequence and each must have a caption. References are to be cited in the text by giving the author’s name and year of publication. References in the reference list should follow the preferred method of quoting references to books, periodicals, reports and theses, etc., and be listed alphabetically by author and then chronologically by date. Abbreviations of titles of periodicals shall be in accordance with the International Standard Organization 1S04 “International Code for the Abbreviation of Titles of Periodicals” and International Standard Organization 1S0833 “International List of Periodical Title Word Abbreviations” and as amended. Appendices should be placed at the end of the paper, be numbered in Arabic numerals, have a caption and be referred to in the text. Reprints. An author who is a member of the Society will receive a number of reprints of his paper free. An author who is not a member of the Society may purchase reprints. 308 4876 | S; f Vi 7 iB