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Volume II, Number 12 August, 1981

Occultation Newsletter is published by the International Occultation Timing Association. Editor and Compositor: H. F. DaBo11; 6 N 106 Whit2 Oak Lane; St. Charles, IL 60174; U.S.A. Please send editorial metters to the above, but send address changes, requests, matters of circulation, and other IOTA business to IOTA; P.0. Bo-x 596; Tiniey Park; IL 60477; U.S.A.

FROM THE PUBLISHER John Phelps reports that the IOTA treasury balance stands at about $2000, so that no membership or ba- For subscription purposes, this is the second issue sic subscription price increase will be needed this of 1981. year, in spite of general inflation and substantial postal rate increases. The only increase (last one o.n.'s price is $1/'issue, or $4/year (4 issues) in- on January I) is the extra price paid by overseas m eluding first class surface mailing, and air mail to non-IOTA o.n. subscribers for airmail delivery. Mexico. Back issues also are priced at $1/issue. Please see the masthead for the ordering address. Some members have suggested that IOTA incorporate as Air mail shipment of o.n. subscriptions is $1.80/yr. a non-profit organization; some advantages of doing extra, outside the U.S.A., Canada, and Mexico. this are described below. Our inclination now is to incorporate, but before we do so, we will give you a IOTA membership, subscription included, is $7/year chance to express your feelings about it, pro or for residents of North America (including Mexico) con, by writing to me or to the IOTA address in Tin- and $9/year for others, to cover costs of overseas Icy Park, IL. More about this will be reported in air mail. European and U. K. observers should join the next issue. Many local astronomical societies IOTA/ES, sending DM 12.-- to Hans J. Bode, Bartold- smaller than IOTA have incorporated. The cost to Knaust Str. 8, 3000 Hannover 9], German Federal Re- incorporate in the State of Illinois is $75, plus a public. fee for a lawyer to prepare the necessary papers. We could incorporate in another state, and would es- IOTA NEWS pecially consider doing so if one of you, or a friend, is a lawyer willing to do the paper work at David KL Dunham little or no cost to IOTA. After incorporation, we will file an application with the Federal government I plan to attend the Astronomical League/A.L.P.O. as a non-profit organization to obtain tax-exempt Convention, "AstroCon 81," at Kutztown State College, status. This will permit us to do several things, Kutztown, PA, at least for the paper sessions on including the following: We will be able to write August 13 and 14, and workshops on the ]5th. I plan proposals to obtain grants to purchase equipment or to give a paper on recent IOTA work, during which I to hire part-time help to finish some of IOTA'S plan to show movies of the 1980 February 16 total long-languishing projects. Members can deduct their k~. solar eclipse which we made near the southern limit IOTA expenses from their reported income on federal in India, and of the May 9th grazing occu1tatiori tax returns. Besides membership dues, these expens- videotape discussed on p. 166. The paper may be es can include the cost of travel to observe grazes given during the International Amateur-Professional and other occultation events, the purchase of spe- Photoelectric Photometry (IAPPP) paper session the cial equipment to be used for IOTA work, and part of afternoon of the 14th. I have also requested a your rent or mortgage payments according to the ra- workshop on occultations the next day, probably to tio of the number of square feet of your dwelling be held, totally or in part, concurrently with the devoted to IOTA records and equipment, to the total IAPPP photometry workshop in the afternoon. An number of square feet of your dwelling. We can ob- IOTA/Nationa1 Capital Astronomers (the local Astro- tain a reduced domestic bulk mailing rate. These nomical League affiliate, of which I am a membCr) things will not help foreign IOTA members directly, display is also planned. Graham Blow, who has or- but even they will benefit from the increased IOTA ganized photoelectric occu1tation observations and services which can result from incorporation. Oc- is director of the very active Occultation Section cultation observers in other countries might obtain of the Royal Astronomical Society of New Zealand, similar benefits by forming their own national or- will be travelling in the U.S.A. at the time and ganization. Effectively, some already have done plans to attend AstroCon 81. It should be a useful this by establishing occultation sections of larger convention for occultation observers. incorporated national astronomical associations. Tax deductibility for travel alone would encourage Unfortunately, tests of the relatively inexpensive more graze, and other occultation, expeditions, occultation photometer described on p. 129 of the which should result in more observations. last issue are behind schedule. Those interested in assembling a copy of the photometer should write for This issue has been delayed by my work with eclipses infomation to Peter C. Chen, Department of Astrono- and asteroid occultations. Besides work for the new my, University of Texas, Austin, TX 78712, U.S.A. 1981 events, I have completed preliminary calcula- 156 "* . tions for all of the 1982 planetary/asteroida1 oc- added, including a short one on occultations by as- cultations to meet a deadline for the Handbook of teroids. A Foreword has been written by Dr. john the Royal Astronomical Society of Canada. The usual O'Keefe. The first edition was reviewed in Sky and articles about observed grazes and new double stars Telescope, 51 (3), 189, and in o.n. i (7) 63. IOTA will be delayed until the next issue, which we plan members can obtain the new edition at a 10% discount to distribute within four to six weeks. Renewal ($8.10) by sending a check payable to the author at notices are included for many with this issue, and the above address. prompt payment (before distribution of the next is- sue) is encouraged. A meeting of IOTA/European Section is planned to be held in Hannover, on Saturday, November 7th. De- Working with Alan Fiala and Tom Van Flandern at tails may be obtained by writing Hans-joachim Bode, USNO, I have developed software to compute automati- Bartold-knaust Str. 8, 3000 Hannover 91, Geman Fed- cally the latitudes and times of points at equal in- eral Republic. tervals of longitude in the northern and southern limits of total and annular eclipses, taking into 1977 TOTAL OCCULTATION TALLY account the lunar valleys and mountains according to joseph E. Carroll Watts' data, as well as numerous other factors con- sidered by Van Flandern in his analysis of occulta- The following two tables — one by country and one by tion data. The path of the july 31St total ec1i,pse was computed and plotted on fairly detailed, re- individual — present the ordered counting of total stricted maps of the U.S.S.R. Descriptions of sites occultations reported for the year 1977. In the in- just inside the path edges were sent to potential dividual lists, it appears that the first three en- observers, who probably do not have access to topo- tries derive from multiple observers. The leading graphic maps themselves. \Ae hope that some observa- lone observer, therefore, is Morrisby from Rhodesia, tions will be made which will be useful for measur- followed closely by Hays of the U.S.A. X...- ing the solar radius. Alan Fiala is taking video equipment to Bratsk, Siberia, where he hopes to re- The values again were computed as in 1975 and 1976 — cord Bailey's beads from a site near the northern via the formula: Value = Total + C x Reappearances, limit. Hans Bode is traveling to Tselinograd, where where C is the ratio of total disappearances to to- he plans to make observations near the southern lim- tal reappearances minus 1. In 1977, 471 observers it. Our preliminary analysis of the Australian ob- from 32 countries reported 9038 total occultations, servations made near the edges of the path of annu- of which 2135 were reappearances. That makes C = 1arity of last February's eclipse gives a solar ra- 2.2333, or reappearances are weighted over disap- dius exactly the same as that we determined from our pear- 1980 February total eclipse timings in India. I am ances by 1977 TOTAL OCCULTATION RANKING BY COUNTRY starting to analyze graze observations to try to im- the fac- prove knowledge of the lunar profile at small lati- tor " Rank Value T,o,t,a.1, B's Country # Obs. tude Vibrations, and will report on this work in the 3.2333. next issue. 1 4532.5 2824 765 United States 85 In the 2 1928.2 1084 378 japan 33 David Herald reduced Astrographic Catalog data to table of 3 990.2 854 61 Australia 24 obtain the positions of faint non-SAO stars in the individ- 4 792.9 449 154 Rhodesia 3 field traversed by the partially eclipsed moon on ua1 ob- 5 749.2 575 78 England 34 July 17. I created a small special USNO "B" cat- servers, 6 748.4 380 165 Denmark 13 alog from Herald's data and computed occultation numerous 7 725.2 455 121 U.S.S.R. 70 predictions during the July eclipse, which I dis- blanks 8 664.1 519 65 New Zealand 31 tributed to photoelectric observers, most of them occur 9 422.3 266 70 South Africa 5 in the U.S.A. Because the eclipse was only par- for 10 306.4 197 49 Argentina 3 " tial, only those with access to large telescopes names 11 258.1 180 35 Belgium 9 _ had a reasonable chance to time the occultations of where 12 233.9 187 21 Germany 21 the non-SAO stars. Don Stockbauer reports that he none 13 190.7 117 33 Philippines 4 and another observer successfully timed the graze were 14 159.3 128 ]4 Czechoslovakia 45 of an 8.0-magnitude SAD star under clear skies dur- availa- 15 156.6 141 7 Netherlands 13 ing the eclipse in Mississippi. ble. In 16 ]37.9 62 34 Canada 7 some of 17 120.6 96 11 Portugal 5 Dr. Kubo reports that the International Lunar Occul- these 18 114.4 101 6 Italy 12 tation Centre plans to produce computer-generated cases 19 113.0 84 13 Brazil 8 maps of occultation limits for 1983 on, for various (notably 20 100.0 62 17 Spain 6 publications. The Royal Greenwich Observatory did the Sim- 21 98.7 63 16 Switzerland 3 this previously, and has distributed maps for 1982, osato 22 90.9 73 8 Austria 20 the last year for which they produced the maps. and Sir- 23 64.9 47 8 Norway 5 Michael Kazmierczak modified his copy of the IOTA ahama 24 25.0 25 0 jugoslavia 1 graze prediction program to generate path data on observa- 25 17.5 13 2 Finland 3 magnetic tape, which he then used to produce maps of tories 26 17.2 15 I Namibia I graze paths crossing GA, SC, and NC, automatically. in ja- 27 16.2 14 i Scotland 2 pan) the 28 9.2 7 I Israel I Harold R. Povenmire, 215 Osage Dr., Indian Harbour 1oca- 29 9.0 9 0 Chile 1 Beach, FL 32937, U.S.A., has written a second edi- tions 30 5.2 3 1 Sweden 1 tion of his Graze Observers Handbook, containing 180 are the 31 5.0 5 0 Iraq 1 pages and illustrated with 15 pictures and charts. same. 32 3.0 3 0 Mexico 1 In a few places, changes have been made from the The rep- original edition, and some new chapters have been etition Totals 9038 2135 471 .. . G 157

e %0 is based upon differing observer codes in the Royal Greenwich Observatory tape data. [continued overleaf]

RNK VALUE QB3ERVER LOCATION TCIIALRUP UKVALUE OBSERVER LOCATION TOTAL REAP

1 624.9 JA PAN, SIRAHAKA 357 120 m 26.9 J. A. BARRATA ARAUJQ BRAZIL, RECIFE 9 8 2 523.7 WEIT&-KNU1JSEN, ET AL DENMARK. TISVILDELEJE 206 142 108 26.7 NOEL MLMFORD NW ZEALAND, PALMERSTON NOR. 20 3 3 507.7 J AFRICANO ET AL U .S. A. , mDoNALD ®S. TEXAS 367 63 109 26.6 T HIRAWA JAPAN. KURASIKI 11 7 u 433.3 A NORRISBY RHODESIA, SALISBURY 219 96 110 26.4 J BELGIUK, BRUSSELS, R. 083. 13 6 5 399.6 R HAYS JR. U, S. A. , CHICAGO. ILLINOIS 192 93 111 26.2 JAME3 H. FOX U.S.A., WEST ST. PALM MINN, 24 T 6 340.5 DAVID HERALD AUSTRALIA. CANBERRA 240 45 112 26.2 F CERCEIIO ITALY, RIVALBA, NR. TWIN 2U 1 7 318.6 T TAKEMURA JAPAN, KURASIKI 169 67 113 26.0 M THQNLAS NEld ZEALAND, DUNEDIN 26 0 8 265.2 JAN HERS S. AFRICA, RAXDCURG 129 61 11u 26.0 id. H. ROBERTSON AUSTRALIA, SYDNEY OBSERVATORY 26 0 g 259.8 J VINCENT RHODESIA, SALISBURY 137 55 115 25.4 JAPAN, KURASIKI 12 6 10 254.3 JAMES L. FERREIRA U. S. A. , FRUO(T, CALIF. 136 53 116 25.2 NEV ZEALAND, AUCKLAND 23 i 11 236.2 ROBERT CLYDE U. S.A. , STREETSBORO, OHIO 100 61 117 25.0 V PRCYTIC-BENISEK YUGOSLAVIA.. BELGRADE OBS. 25 0 12 231.7 WALT MORGAN U .S. A., LAS VEGAS, KEVAN 91 63 118 24.5 J RYDER AUSTRALIA, BRI3BANE 20 2 73 279.6 RICHARD NQLTHENIUS U.S.A., su DIEGO, CALIF. 166 2U 119 24.2 KLAUS KLEBERT GERMNY, STUTTGART SldABIAN 22 1 14 194.u ROBERT H. SANDY U .S.A., KANSAS an, KISSOURI ?14 36 iaj 24.0 EZEQUIEL CABRITA PORTUGAL, LISBON OBSERVATORY 2U 0 ?5 193.4 DON IQ. STDCKBAUER U. S. A. , VICTORIA, TEXAS 113 36 121 23.9 Id MELLOR ENGLAND, smFIELD 15 4 16 170.u ROBERT LASCR U.S.A., GREEN VALLEY ARIZCMA 99 32 122 23.7 A SALAZAR SPAIN, SAN FERNANDO OBS. 17 3 ¶7 161).6 JOHN S. KORINTUS U.S. A. , PALM BAY, FLORIDA 107 2U 123 23.5 d mis EUGLAKD, BIRMINGHAM 19 2 18 159.7 B. SINCHESKUL U. 3. S. R. , POLTAYA 86 33 124 23.2 U,S,A., ROCKLEDGE, FLORIDA 21 1 19 148.0 P ANDERSON AUSTRALIA. BRISBANE jug 0 125 23.2 NORWAY, LAMGENESBYGDA 21 1 20 1UU.2 J RODRIGUEZ ARGENTINA, CORDOBA CBSERVATORY IOU 18 126 23.2 CARL GRUNNET DENKARK. VIRUK 21 1 21 1U1.5 JA PAN, SIRAHAMA 79 28 727 23.0 AUSTRALIA. CHINCHILLA 23 0 22 134.'1 JAPAN, SIMOSATO 54 36 128 22.9 WILLIAM J. WESTBROOKE U,S,A,, SAN FRANCISCO, CALIF. 14 4 23 133.3 JAPAN, SIRAHAKA 73 27 129 22.9 E KARKQSCHKA GEDUNY, STUTTGART 14 a 24 131.0 K BLACKidELL EKLAJID, jdESTHA!8, SUSSEX 93 17 130 22.2 A. FOROSHIN U.3.S.R., GORKI 20 1 25 126.7 BEN HUDGENS 1J,S,A,, CLINTON, MISSISSIPPI 82 aj 131 22.2 A MCCMNELL U.S.A., RIDGECREST, CALIFORNIA 20 i 26 123.6 AMBROSIO JUAN CAMPONOVO ARGENTINA, BUENOS AIRES 70 2U 132 22.0 AUSTRALIA. LAYINGTON 22 0 27 }22.0 STEVE J. ZVARA U. S. A. , WITTIER. CALIFORNIA 55 30 733 21.9 ITALY, TURIN 73 u 28 121.2 OSCAR G. IE LAS ALAS PHILIPPINES, KANILA 52 31 134 21.9 ROLAND BCNINSEGNA BELGIUM, CHARLER0I(KARCINELLE) 13 u 29 117.7 lq bech demmark, copenhagen 73 20 135 21.7 V. SINCKESKUL U.S.S.R., POLTAVA 15 3 30 117.6 JEAN BOURGEOIS BELGIUM, MONTIGNY LE TILLEUL 64 24 736 21.2 ENGLAND. HARROGATE 19 1 31 117.3 DOUGLAS HALL ENGLAND. LEICESTER 57 27 137 21.0 U.S.A., ENGLEWOOD, FORIDA 21 0 32 177,1 E HALBACH U .S. A. , PQIUdAUKEE. WIS. 59 26 138 21.0 J BAGULEY ENGLAND, DERBY 21 Q 33 1)4.8 U .S. A. , MORONGO VALLEY, CALIF. 50 29 139 20.7 H TWIOKA JAPAN, HITACHI 14 3 3U 112.2 DAVID D. BROW CANADA, MONTREAL U3 31 iud 20.5 R MIDDLETON ENGLAND, COLCHESTER 16 2 35 100.0 GEORGE WINGATE KEY ZEALAND, AUCKLAND 62 17 1Ul 20.2 OCENAS CZECH., BANSKA BYSTRICA 9 5 36 99.7 A HILTON RHODESIA, SALISBURY 93 3 1U2 20.0 F ROSSET ITALY, UDINE 20 0 37 95.8 JAPAN, SWCSATO 40 25 1U3 19.9 AWTRIA, ST LEONHARD(POLTEN) 11 u 38 87.0 JAPAN, KURASIKI OBS. 58 13 1UU 19.5 ENGLAND, EASTHAM 75 2 39 84.6 ALFREDINA DO CAMEO PORTUGAL, LISBON OBSERVATORY 60 11 1U5 19.u NETHERLAND3, ZOETERMEER 6 6 '10 83.2 KICHAEL C. ASHLEY AUSTRALIA, CANBERRA 72 5 146 19.2 V TANNEY U.S.A.. MILWAUKEE, VIS. 8 5 '11 83.0 JAMES H. VAN NULAND U.S.A., SAN JOSE, CALIF. 83 Q 147 19.0 AUSTRALIA. PERTH OBSERVATORY 19 0 uz 82.2 JOSEPH E. CARROLL U ,S.A. , MINNETONKA, MINNESOTA u2 18 jug 18.5 N FRASER ENGLAND, LEICESTER 14 2 43 82.0 CLIFFORD J. BADER U. S. A. , WEST CHESTER, PA. uu 17 149 18.2 H LUFT U.S.A.. OAKLAND GARDEN3, N.Y. 16 7 4U 8¶.0 PAUL ASIQUS U. S. A. , AURORA, COLORADO 52 13 150 18.2 C KAPRAL U.S.A., PARLIN NEW JERSEY 16 1 45 78.7 LIONEL E. HUSSEY HEM ZEALAND. CHRI3TCHURCH 34 20 151 18.2 NETHERLANDS. STREEKERK 16 1 '16 78.2 GLEN ROWE NEJQ ZEALAND, AUCKLAND 76 1 152 18.2 0 KLIjrTIjjG DENMARK, RINGSTED 76 T 47 72.8 U .S.A,, DENVER, COLORADO 46 12 153 18.0 JAMES FERILLAT U.S.A., OAKLAND, CHABUT OBS. 18 0 U8 71.7 H. F. COCHRAN U .S. A. , BRCMMdOOO, TEXAS 65 3 15U 18.0 R BOSCKOO NETHERLANDS, LAREN 18 0 49 69.9 G MARSHALL S. AFRICA. JOHAMESBURG 61 u 155 18.0 JAPAN, TIBA 18 CI 50 67.7 PAUL J. NEYKAN U ,S, A. , GARLAND, TEXAS 23 20 156 18.0 0 CHAVES BRAZIL, RIO DE jANEIRO 18 0 51 66.2 ROGER LAUREYS BELGIUM, DIEPEKBEEK 6u 1 157 18.0 B BRIDGE AUSTRALIA. BRISBANE 18 Q 52 65.2 AUSTRALIA, CANBERRA SU 5 158 17.2 E SAWYER NAMIBIA, WINDHOEK 15 1 53 63.7 A. ZHITETSKI U.S.S,R., KIEV 28 16 159 17.2 N WATANABE JAPAN, SIMOSAT'O 6 5 su 63.0 F ZEHNDER SldITZERLAKD, BIRIQENSTORF y 13 160 17.0 J MEDSKER U.S.A., BUCHANAN, MICHIGAN 17 0 55 61.5 JUAN D. SILVESTRE PHILIPPINES, MANILA 57 2 161 17.0 A VAN DER NIFT NETHERLANDS, SOESTDIjK 17 0 56 60,0 J SMITH U.S.A., WACO, TEXAS 60 Q 162 16.9 E NISIKURA JAPAN, TOKYO 8 u 57 59.5 H. F. DABOLL U. S.A. , ST. CHARLES, IL. 26 15 163 16.5 U.S.A., URBANA,ILLINOIS UNIV. 12 2 58 56.8 0. KVARATSKHELYA U. S. S. R. , ABASI1MANI OBS. 30 12 164 16.5 AUSTRIA, VIENNA 12 2 59 5U.9 Y KINOTO JAPAN, TOKYO 46 u 165 16.2 A. YUSHCHUK U.S.S.R., KIEV 5 5 60 54.8 SPAIN, SAN FERNANDO OBS, 28 12 166 16.2 L BRUNDLE ENGLAND, HANARDS HEATH 14 1 61 53.2 V. NAZUR U.S.S.R., KIEV U2 S 167 15.5 V. F'HEDQSENKO U.S.S.R., KCMSOMCLSK-NA-AMUR 11 2 62 52.5 ALFRED C. WEBBER U.S. A. , CHADW FORD, PA. 08 2 168 15.5 JOSE OSORJO SPAIN, KADRID 11 2 63 51.0 B SOULSBY AUSTRALIA, CANBERRA 51 0 169 15.5 KATTI SUHONEN FINLAND, HELSINKI 11 2 64 49.1 HANS-JOACHIM BODE GERULNY, RAKNOVER 29 9 170 15.2 U.S.A,, CHICAGO. ILLINOIS 13 1 65 u6.5 MARK GINGRICH U.S.A. , OAKLAND, CEIABOT OBS, u2 2 171 15.0 BARRY MENZ JES NE\1 ZEALAND, AUCKLAND 15 D 66 u6.5 RICHARD BINZEL U.S. A. , MACALESTER COLLEGE, lqN Q2 2 172 75.0 V RASMUSSEN DENMARK, KDLDING 15 I) 67 uu.8 k kenmwu japan, sn«mTo 18 12 773 74.2 SCOTLAND, DUNDEE, MILLS OBS. 12 1 68 uu.0 J VAN DER MEULEN NETHERLANDS. ldQGKUM uu 0 174 ¶il2 ITALY, ROME 12 1 69 '13.9 S. AFRICA, JOHANNESBURG 35 El 175 1u.2 C BRUNT ENGLAND, CAMBRIDGE OBS. 12 1 ~ 70 '13.2 MAURICE STOKER NEW ZEALAND. AUCKLAND 32 S 176 1u.2 ENGLAND, WIKBORNE 12 1 71 39.9 GERRY ALLcwr NEV ZEALAND, AUCKLAND 31 u 177 14.0 U.S.A., SOLON, OHIO 14 0 72 39.6 V. KAZHOROVSK1 U. S. S. R. , POLTAVA 15 11 178 1U.O H KRUIQB S. AFRICA. LANGEBAAN 14 0 73 39.3 A. QSIPQV U.S.S.R., KIEV 17 IQ 179 14.0 J. VAN CAMP BELGIUM, URANIA OBS. 14 0 74 39.0 h. williams ma zealand, auckland 39 0 IBO 1u.0 MARK TAYLOR AUSTRALIA, CANBERRA 14 0 75 38.7 JORGE POLMAN BRAZIL, RECIFE 32 3 181 13.7 C CAWON JR U,S.A,, SAN FRANCISCO, CALIF. 7 3 76 38.6 EDUARDO VALENTIN PRZYBYL ARGENTINA. RAFAELA 23 7 182 13.? M KAYADA , JAPAN, TOKYO 7 3 77 38.5 A MAUONALD AUSTRALIA, TCM©YILLE 3u 2 183 13.5 JAPAN, TOKYO 9 2 78 37.7 GRAHAM L. BLAH NEJI ZEALAND, AUCKLAND 31 3 18U 13.5 ENGLAND, BIRMINGHAM 9 2 79 36.7 H ABE JAPAN. QSYAMAMBE 30 3 185 13.2 KARTIN KNITSCH GERMANY, HANOVER 11 1 go 36.6 PI. ESIMATOV U .S. S. R. , TASHKENT 12 11 186 13.0 V. GOLUBEV U.S.S.R., GORNO'TAEZHNI, SIBERIA 13 0 81 36.6 TOM BUTLER U.S.A., TROY, MISSOURI 21 7 187 13.0 A WELLS ENGLAND, BIRMINGHAM 13 0 82 35.5 D PETTITT ENGLAND. CARLISLE 31 2 188 12.5 A. KOROZOV U.S.S.R., TCNSK 8 2 83 35.5 G MORSE ENGLAND, MIDENHEAD 31 2 189 12.2 U.S.A., SAN FRANCISCO UNIV. 10 1 84 3U.6 ROBERT N. BOLSTER U.S. A. , ALExAmIA, VA. 79 7 190 12.0 CHRISTOPHER STEPHAN U.S.A.. STREETSBORO, CHlO 12 0 85 34.2 DAVID BROCK NEld ZEALAND, AUCKLAND 32 1 191 12.0 GERKANY, SCWIDEN/STUTTGART 12 0 86 3u.2 NEW ZEALAND. GISBORKE 32 1 192 12.0 P DARNELL DENMARK, COPENHAGEN 12 0 87 33.7 G HEJdICK ENGLAND. LEICESTER 27 3 193 12.0 DENMARK, COPENHAGEN 12 0 88 33.0 AUSTRALIA, BRIWAIIE 33 0 19U 11.5 N TABEISI JAPAN, TOKYO 7 2 89 32.9 HARALD MARK G£NAJ{Y, KORKTAL-MUNCHINGEN 24 4 195 11.5 JAPAN, TOKYO 7 2 go 32.7 ROBERT GERKANM SWITZERLAND. WALD 26 3 196 11.5 ENGLAND, WALES, DYSERTH 7 2 91 32.7 j pogoda czechoslovakia, ol.aqouc 26 3 197 11.5 KARL E. MCNAMARA CANADA, MONTREAL 7 2 92 32.6 JOSEPH ZODA U. S. A. , MAPLE PARK, ILL, 17 7 198 17.2 VICTOR J, SLABINSKI U.S.A., ARLINGTON, VIRGINIA 9 1 93 32.4 0 MIDTSKOGEN NOWAY, TRAKBY 19 6 199 11.0 ROBERT R. BAILEY U.S.A., HOUSTON, TEXAS 11 0 94 31.4 U. S. A. , LAKE PARK, FLA. 78 6 ZOO 11.0 E UTTO GERMANY, EILENBURG 11 Cl 95 31.2 GEOFFREY Id. AMERY ENGLAKD, READING 29 1 207 10.5 BRAZIL, RECIFE 6 2 96 31.0 D. STANKEVICH U. S.S. R. , KHARKOV 31 0 202 10.2 V. TKACHENKO U.S.S.R., KHERSON 8 I 9? 31.0 J MCMGAN ENGLAND, CAMBRIDGE OBS. 31 0 203 10.2 G KELLOCK AUSTRALIA. CANBERRA 8 1 98 30.2 H PACHALI GERMANY, BERLIN NEUKOLLN 28 1 2OU 10.0 U.S.A.. MCMINNVILLE, TENNESSEE IQ 0 99 30.2 ENGLAND. BRACKNELL 79 5 205 10.0 D SCWIUF NETHERLANDS. HUIZEN IQ 0 100 30.2 ROGER H. GILLER AUSTRALIA, ENGADINE 28 I 206 9.7 G SAMCLYK U.S.A., MILWAUKEE. WIS. 3 3 101 30.0 BRUCE RU3NAK U.S.A., ST. PAUL, MINNESOTA 30 0 207 9.5 D SCOTT U.S.A., PAKAKA CITY, ELOHIM 5 2 102 29.6 JAPAN, SIMOSATO 14 7 208 9.2 G. HERDMAN NEV ZEALAND, AUCKLAND 7 1 103 29.2 CHET PATTON III U .S. A. , BUCHANAN, MICHIGAN 18 5 209 9.2 M ALON ISRAEL, YAVNE 7 1 104 29.2 L PAIZI S. AFRICA, NIGEL, TVL. 27 1 210 9.2 YEYRICH GERMANY, EILENBURG 7 1 105 27.9 U.S.A. , DUBLIN, CALIFORNIA 19 LI 211 9.2 Id CAUNTER ENGLAND, TONES DEVON 7 7 106 27.6 RONALD Id. CROSS NW ZEALAND, CHRISTCHURCH 12 7 212 9.0 P. PAVLENKO U.S.S.R.. KHARKOV 9 (I 158

Looking over the 1975, 76, 77 lists shows that Hays of the U.S.A., Sirahama Observatory of Japan, and Take-

RNK VALUE OBSERVER LOCATION TOTAL REAP RNK VALUE OBSERVER LOCATION TOTAL REAP

213 9.0 A PENNEL NEW ZEALAND. DUNEDIN 9 0 319 3.0 U.S.A., SATELLITE BEACH, FLA. 3 0 21U 9.0 NETHERLANDS, LEE1NABD£N 9 0 320 3.0 TH(MAS H. CAMPBELL JR U.S.A.. Temple TERRACE, FLA 3 0 215 9.0 JAPAN, NISITAMA 9 0 321 3.0 BEAT RYKART SWITZERLAND, ILATHAL 3 0 216 9.0 T HAJMES ENGLAND, MAIDENHEAD 9 0 322 3.0 M IE PASCUAL KARTINEZ SPAIN, MADRID OBSERVATORY 3 0 217 9.0 ENGLAND, SALFQRD 9 (I 323 3.0 NAZARETH REGGI PORTUGAL, PORTO UNIV. OBS. 218 9.0 E. OTTO CZECH., EILENBURG 9 D 32U 3.0 D YGLOPAZ PHILIPPINES, MANILA . 3 0 219 9.0 M LOOCKS-VASQUEZ CBILE, VALPARAISO 9 0 325 3.0 ROSA TYSON NEW ZEALAND, AUCKLAND 3 0 220 9.0 AUSTRALIA. PERTH OBSERVATORY 9 0 326 3.0 NETHERLANDS, WIGHT 3 0 221 9.0 AUSTRALIA, SYDNEY OBSERVATORY 9 D 327 3.0 F DIEGO MEXICO, MEXICO D.F. 3 0 222 8.5 PAT HARVEY U,S,A., HACIENDA HEIGHTS, CAL. u 2 328 3.0 JAPAN. YOKOHAMA 3 0 223 8.2 A. RAKHIMOV ABWMALIK U.S.S.R., TASHKENT 6 1 329 3.0 JAPAN, TOKYO 3 0 22U 8.2 JAPAN, TOKYO 6 1 330 3.0 ITALY, MILAN 3 0 225 8.2 K SILBER AUSTRIA, GMUNDEN 6 } 331 3.0 ITALY, ANCONA 3 0 226 8.0 JOHN A. CHURCH JOSE U.S.A., PRINCETON JUNG., N.J. 8 0 332 3.0 GERKANY, RUDOLSTADT 3 0 227 8.0 QSORIO PORTUGAL, PORTO UNIV. OBS. 8 Q 333 3.0 E SPLITTGERBER GERMANY, SONNEBERG OBS. 3 0 228 8.0 JAPAN. TOKYO 8 CI 33U 3.0 A HOUSKA CZECHOSLOVAKIA. TURNQV CZECH., 3 0 229 8.0 ITALY, TURIN 8 CI 335 3.0 P NAJ3ER PRAGUE PEOPLE'S OBS. CZECH., 3 0 230 8.0 AUSTRIA, GRAZ 8 0 336 3.0 SOJKA SUCHAN PRAGUE PEOPLE'S OBS. CZECH.. 3 0 231 7.5 M MORRCAd U.S.A., HAWAII, OAHU EldA BEACH 3 2 337 3.0 FIEDLEROVA PRAM 3 0 232 7. 2 JAMES E. BROOKS H U.S.A., CHATHAM, VIGINIA 5 ' 338 3.0 VOLF CZECH., PRAM 3 0 233 7.2 POVENIQIRE U.S.A.. SATELLITE BEACH, FLA. 5 1 339 3.0 CZECH., PRAM 3 0 234 7.2 D HOUGH U.S.A., SOUTH PLAINFIELD 5 1 340 3.0 CANADA, VICT. DOMINION OBS 3 0 235 7.2 DENMARK, VIBY, JUTLAND 5 1 341 3.0 AUSTRIA, ST. FOLTEN 3 0 236 7.0 B. M. LEWIS E BEET NEV ZEALAND, YE., CARTER OBS. 7 0 342 3.0 AUSTRIA, VIENNA 3 0 237 7.0 ENGLAND. ASHAMPSTEAD ENGLAND, 7 0 343 3.0 AUSTRIA. VIENNA 3 0 238 7.0 J OLESEN SHEERNESS 7 0 34'1 3.0 E LUMLEY AUSTRALIA, SYDNEY 3 0 239 7.0 A. ZAPOROZHETS DENMARK. RONNE BORNHOLM 7 0 345 3.0 AUSTRALIA, GEELONG 3 0 2 0 2UO 6.5 ZIMNIKOVAL U.S.S.R., ODESSA 2 2 346 2.0 A. EPHIMOV U.S.S.R.. RIZAN 2 0 241 6.5 A. SHAPOVALOV CZECH., BANSKA BYSTRICA 2 2 3u7 2.0 V. A. VOROTNIKOV U,S.S.R., ENISEICK123 242 6.2 S. IEMAYLOV u 1 348 2.0 A. KHOLODNI 2 0 U.S.S.R,, KHERSON U.S.S.R.. GORKI 0 243 6.0 G DELAHUNTY lj.S.S.f., KHARKOV 6 a 3U9 2.0 I. MUSIKHIH U.S,S.R., GORKI 2 &_ 0 2 2UU 6.0 U.S.A., GARDEN CITY, N.Y. 6 0 350 2.0 V. KHAREVICH U.S.S.R., ENISEISK 0 245 6.0 WAYNE CLARK U.S.A., MILWAUKEE, VIS. 6 0 351 2.0 N. KRASNIKOV U.S.S.R., KAZAN 2 0 246 6.0 U,S.A., ST. LOUIS, MISSOURI 6 0 352 2.0 0. ORLOVSKI U.S.S.R., KRASNOYARSK 2 0 2U7 6.0 H KRUGER JAPAN, YOKOHAMA 6 0 353 2.0 P. VELESHCHUK 1J.S,S.R., KIEV 2 0 248 6.0 E AHNERT GERMANY, HANHOVER 6 0 354 2.0 M. P'YSHNENKO U.S.S.R.. KHABAROVSK 2 0 2U9 6.0 S PATTINSON L GERMANY, SONNEBERG OBS. 6 (I 355 2.0 V. VELMU$HK[N U.S.S.R.. K!1ERSON 2 D 250 6.0 MORRISON ENGLAND, SOUTH CROYDON 6 e 356 2.0 P. KOSYARUM U.S.S.R., CHERKASSI 2 D 251 6.0 V HAUT ENGLAND, WESTHAM, SUSSEX 6 CI 357 2.0 V. KIKHHO U.S.S.R., CHERKASSI 2 0 252 6,0 CZECHOSLOVAKIA, CHEB 6 0 358 2.0 R ROVER U.S,A., YRIGHNOOD, FORD OBS. 2 0 253 6.0 JEAN MEEUS BRAZIL. RIO DE JANEIRO 6 Q 359 2.0 U.S.A.. BALTIMORE, MARYLAND 2 0 25'1 6.0 K. P. SIMS BELGIUM, ERPS-KJBERPS 6 (I 360 2.0 U.S.A., COCOA, FLORIDA 2 0 255 6.0 N BUTTERWORTH AUSTRALIA, SYDNEY OBSERVATORY 6 0 361 2.0 P KURN U.S.A., MILHAUKEE, VIS. 2 0 256 6.0 V. ILIN AUSTRALIA, TOWKSVILLE 6 0 362 2.0 SPAIN, MADRID OBSERVATORY 2 0 257 5.2 I. BLAGOVESHCHENSKI U.S.S.R., KAZAN 3 1 363 2.0 R EBERST SCOTLAND, EDINBURGH 2 0 258 5.2 ROGER ERIKSSON U.S.S.R., ULYANOVSK 3 1 364 2.(J R GLEDHILL NEW ZEALAND, DUNEDIN 2 0 259 5.2 G. PATTERSON F SWEDEN, LUND 3 1 365 2.0 G. COULING HE1d ZEALAND, WELLINGTON 2 0 260 5.2 PAVLAS NEld ZEALAND, CHRISTCHURCH 3 1 366 2.0 NETHERLANDS, GOUTIRQ 2 0 261 5.2 M. MULLER CZECHOSLOVAKIA, HOLESOV 3 I 367 2.0 H BETLEK NETHERLANDS. LEIDEN 2 0 262 5.2 CZECH., EILENBURG 3 ' 368 2.0 JAPAN, TOKYO 2 Cl 263 5.2 V, LAZAREV AUSTRIA, VIENNA 3 i 369 2.0 JAPAN, TOKYO 2 0 26U 5.0 A. ZAPOROZHETS 1J,S.S.R., TOHSK 5 0 370 2.0 ITALY, BOLOGNA 2 0 265 5.0 CESARIQ E. TAGANAS N U.S.S.R., KIEV 5 t) 371 2.0 ITALY, ANCONA 2 0 266 5.0 BRYNILDSEN PHILIPPINES, MANILA 5 " 372 2.0 MULLER WOLFGANG GERMANY, EILENBURG 2 0 267 5.0 E. RANRAM NORWAY, HORTEN 5 0 373 2.0 BEISKER GERMANY, HANNOVER 2 0 268 5.0 NEW ZEALAND, AUCKLAND 5 C 37q 2.0 GEMANY, WIEL-DER-STADT 2 0 269 5.0 NEW ZEALAND, DUNEDIN 5 0 375 2.0 V HEGVAD DENMARK. COPENHAGEN 2 Cl 270 5.0 G OLTHUIS NETHERLANDS, GRONINGEN.KAFTEYN 5 0 376 2.0 M. KATYSEK V CZECHOSLOVAKIA, GOTTldALDOV 2 0 271 5.0 NETHERLANDS, UITHOORN 5 JJ 377 2.0 TALKNER CZECH., JINDRICHOV HRADEC 2 0 272 5.0 ITALY, MILAN 5 0 378 2.0 M. VACLARIK J CZECH.. F'OLICE-MD-METUJI 2 0 273 5.0 M ABDULAHAD R ITALY. ANCONA 5 0 379 2.0 PAVLOUSEK CZECH., PRAGUE PEOPLE'S OBS. 2 0 274 5.0 PICKARD IRAQ. BASRAH 5 0 381) 2.0 MUDRA CZECH., PRAGUE PEOPLE'S OBS. 2 I) 275 5.0 ENGLAND, HADLCAd, KENT 5 e 381 2.0 B MALECEK CZECH,, VALASSKE MEZIRICI 2 (I 276 5.0 K. V. FABRIN E ENGLAND, FLUCKLEY 5 0 382 2.0 PRIBYL CZECH., PRAHA : ggg----- 277 5.0 PEDERSEN 5 0 383 2.0 BUBENICEK CZECH.. PRAM 0 DENMARK. AALBORG 0 278 5.0 J BOCEK DENMARK, HORSENS. JUTLAND 5 0 38U 2.0 PLECHAC CZECH., PRAHA 2 279 5.0 CZECH., JINDRICHOV HRADEC 5 0 385 2.0 id JUTTING CANADA, MONTREAL 2 0—" 280 5.0 BRAZIL. RIO DE JANEIRO 5 0 386 2.0 AUSTRIA, LINZ ,2 0 281 5.0 AUSTRIA, VIENNA 5 0 387 2.0 AUSTRIA, VIENNA 2 0 282 U.2 E. WEYRICH ANDRE JAPAN, TOKYO 2 1 388 1.0 A. BELYAKOV U.S.S.R., KALININ 1 0 283 '1.2 COULCMBE V, KOSTROV CZECH., EILENBURG 2 1 389 1.0 A. D. TARABAKIN U,S.S.R., KALININ 1 0 28U u.2 V. IJTKIN CANADA,, QUEBEC 2 1 390 1.0 A. KANTOROV U.S.S.R., JXJKSK 1 0 285 4.0 D. GALYCH R WOOD U.S.S.R., GORKI 4 D 391 1.0 A. KIRICHENKO U.S.S.R., UZHGOROD 1 0 286 LO U.S.S.R., GORKI 4 0 392 1.0 V. KIRDATOVSKI U.S.S.R., KHARKOV 1 0 287 'LO U.S.S.R.. L'VOV u 0 393 1.0 I. ZHDANCHUK U,S.S.R., CHERNIGOV 1 0 288 'LO M HERBSTRITT SIDNEY U.S.A., COCOA, FLORIDA u 0 394 1.0 T. FOLIZHUK U.S.S.R., CHERKASSI 1 0 289 LO HENDRICKSON U.S.A., COCOA, FLORIDA 4 0 395 1.0 A.T. MAILBAEV U.S.S.R.. KAZAN 1 0 290 11.0 B. A. SINTON U.S.A., OAKLAND, CHABQ'T OBS. u 0 396 1.0 V. KAZAKOV U.S.S.R., GORKI 1 0 291 '1.0 U.S.A., ST. MARYS, PA. u Q 397 1.0 E. XHARITONOVA U.S.S.R., GORKI 1 0 292 'LO U.S.A,, COLUMBUS, OHIO u 0 398 1.0 A. YINOGRADCJV U.S.S.R., GORKI 1 0 293 'LO NEW ZEALAND, GISBORNE u 0 399 1.0 C. VETOSHCHKIN U.S.S.R., GORKI 1 0 29U '1.0 NETHERLANDS, HILVERSIM u 0 UOD 1.0 jq KAZMIERCUK U.S.A., ATLANTIC BEACH, FLA, 1 0 295 LO JAPAN, TOKYO u 0 UO1 1.0 KARL SIMMONS U.S.A., JACKSONVILLE, FLORIDA 1 0 296 u.o ITALY, UDINE u 0 402 1.0 JERRY SEARCY U.S.A., LAS VEGAS, NEVADA 1 0 297 4.0 ENGLAND, EASTBOURNE u 0 403 1.0 GWEIEKEYER U.S.A,, MILWAUKEE, WIS. 1 0 298 LO ENGLAND. EASTBOURNE u 0 'IOU 1.0 R JAMES U.S.A.. MILWAUKEE, WIS. 1 D 299 u.o P. DRABEK CZECHOSLOVAKIA. GOTNALDOV u 0 405 T.O I DE PALLID QUIROS SPAIN, MADRID OBSERVATORY 1 0 300 lo S KOCHAN CZECH., UAR-NAD-HRONCN 4 0 U06 1.0 A FOSS NOWAY, ASKER 1 0 301 1(.0 C REID CANADA, SELKIRK, MANITOBA u 0 407 1.0 TRIXIE STEYART NEhf ZEALAND, AUCKLAND 1 0 302 u.o I MAGALHAES BRAZIL, RECIFE u 0 408 1.0 Id KOHLBACH GERMANY, RAMNOVER FINLAND. 1 0 303 u.o P,C.A, BARETTCI BRAZIL, RECIFE u 0 'tog 1.0 ILMO KUKKONEN HELSINKI ENGLAND. CAMBRIDGE 1 Q 30U u.o DANIELLE BOURGEOIS BELGIUM, MONTIGNY LE TILLEUL u 0 410 1.0 J SHANKLIN OBS. 1 0 305 4.0 G KAMATSCHNIG AUSTRIA, GIQUNDEN 4 0 U11 1.0 G TAYLOR ENGLAND. NEAR HERSTMONCEUX 1 0 306 4.0 AUSTRIA, VIENNA u 0 412 1.0 KRILL CZECHOSLOVAKIA, GOTNALDOV 1 0 307 'LO G READING AUSTRALIA, GEELONG u 0 Ui3 1.0 METELKA CZECHOSLOVAKIA, UHERSKY BROD 1 0 308 LO T. L. MORGAN AUSTRALIA, SYDNEY OBSERVATORY u 0 414 1.0 SPURNY CZECHOSLOVAKIA, KUNZAK 1 0 309 3.2 0. BOGDANOV U.S.S.R., RIZAN 1 1 415 1.0 KRAJCIR CZECHOSLOVAKIA, HLOHOVEC I 0 310 3.2 A. SLITSCHENKO U.S.S.R., KIEV 1 1 U16 1.0 J VACEK CZECH., POLICE-NAD-METUjI 1 0 311 3.2 G, MOSKALEVA U.S.S.R., KIEV 1 I 417 1.0 KREJCI ROSKOVA CZECH., PRAGUE PEOPLE'S OBS. 1 0 312 3.2 HOWARD D. THOMAS U.S.A.. COULEE DAM, WASH. 1 1 U18 1.0 SOBRA CZECH., PRAGUE PEOPLE'S OBS. 1 0 313 3.2 B SORENSEN NORWAY, TRONDHEIM 1 i 419 1.0 LEV KETOPICK CZECH,, PRAGUE PEOPLE'S CBS. 1 0 31u 3.2 CHROKEK CZECH., BANSKA BYSTRICA OBS. 1 1 420 1.0 H.J. WIDIXjP id CZECH., PRAGUE PEOPLE'S OBS. 1 0 315 3.0 V. SHERSTNEVA U.S.S.R., GORKI 3 Q '121 1.0 JASCHEK CZECH., PRAGUE PEOPLE'S CBS. 1 0 316 3.0 V. KONEV U.S.S.R.. ULYANOVSK 3 0 422 1.0 P REINHARD CANADA, QUEBEC 1 0 317 3.0 Id ALBRECHT U.S.A., MILYAUKEE, WIS. 3 JJ 423 1.0 AUSTRIA, VIENNA, KUFFNER OBS 1 0 378 3.0 J KISIEL U.S.A., PALOS OBSERVATORY 3 0 424 1.0 AUSTRIA, VIENNA 1 0

. ., 159

mura of japan are the only consistent top ten lead- before a tally like this can claim to have even a ers. minimum of accuracy. I can estimate that another 400 observations from 1977 can be expected to appear In the countries list, the U.S.A. tops the list by on future tapes. virtue of its large number of observers. It is in- teresting that this list divides quickly into: the The data compilation resulting iii these two tables, top three, four countries in the 700'S, and everyone therefore, contain a considerable amount of detec- else considerably lower. One can examine these in a tive work, guesswork, and just plain arbitrariness! different way, however — by ranking according to Please excuse me for whatever cFrors are thus pro- value per observer. Here, we find that Rhodesia duced. If you'll let me know of the grosser errors, tops the list by far, with a value of 264.3 per ob- I'll attempt a revision. server. Then comes Argentina at 102.1 and South Af- rica at 84.5. japan, Denmark, and the U.S. follow USING THE IOTA/ILOC OCCULTATION REPORT FORMS in the 50'S, the Philippines and Australia in the 40'S, Switzerland at 32.9, and then everyone else. David W. Dunham Czechoslovakia, fourteenth in the main ranking, drops to thirty-first, by virtue of its large number Yoshio Kubo, Director of the International Lunar of observers. The reason for the change of ranking Occultation Centre, has given me some guidelines for becomes obvious from the data. Many observatories including additional information on their report evidently are used by students, resulting in one ob- forms in a letter dated May 15th. No change in the servation per observer (Are these the result of some current forms is needed, but the information below class assignment?). Rhodesia, on the other hand, should be added to the four-page description, Use of has an apparently dedicated trio. form for recording occultation observations, which has been distributed with the forms. \~- The compilations, of course, have not been solely my doing, though I'll take responsibility for the er- Column 39, Personal equation (PE), A: An additional rors. The project was started at the impetus of code can be used: U (Unsubtracted), The following Dave Dunham, who consistently urged its completion. value of the personal equation has not been sub- Tom Van Flandern supplied the USNO tapes which in- tracted from the observed time. This was suggested cluded RGO data. He also forwarded the Czech and by Robert Clyde, Streetsboro, OH, and was an often- Russian publications. I want particularly to ex- used option on the previous ("U. of Texas ed. 2") press my appreciation to Honeywell, Inc. for its IOTA graze report forms. continuing support and encouragement of these tal- lies and of the asteroid occultation predictions. Column 56 (back of form) is devoted to other phenom- Finally, thanks are due to H. F. DaBe11 who was able ena relating to gradual events other than those to fit the tables and text into their proper place listed for Column 35 (which should be left blank if in the newsletter. Column 56 is used). For Column 56, use the follow- ing code numbers: I wish to apologize for taking so long to complete 1 Start of disappearance at dark limb these lists. Dave Dunham first requested that I do 2 End of disappearance at dark limb this in early 1980. The information received, how- 3 Start of disappearance at sunlit feature ever, consisted of magnetic tapes containing obser- 4 End of disappearance at sunlit feature vations for multiple years, the observation forms 5 Start of disappearance at the umbra during lunar filled out by many observers and mailed to Dave, and eclipse the publications of two countries; Czechoslovakia 6 End of reappearance at the umbra during lunar and Russia. The first problem was reading the eclipse tapes. As anyone who tries this can attest, no com- 7 Partial blink (Star doesn't completely disappear) puter seems to be able to produce a tape readable 8 Faint flash (Star doesn't achieve full bril- ¢- easily by another computer. It took literally six liance) months of part-time effort and the combined talents of Honeywell's software people to devise a solution These events no longer need to be written in the which now runs beautifully. comments area, as was specified in the original in- structions, since they now are listed on separate The next delay was caused by the devotion of my ef- lines. Remember that a blink is a disappearance forts to the asteroid occultation prediction task. followed imediately (by 055 or less, so that the This involved breaking up Dave's program into two events can not be timed separately) by a reappear- (now three) programs so as to respond efficiently to ance, while a flash is the opposite sequence, a re- the needs of that area. appearance followed imediately by a disappearance (star "flashes" out in a deep lunar valley bottom). Upon returning to the tally problem, the second ma- jor difficulty was encountered — no or little cor- Column 57 (back of form) is devoted to D/B/U. Enter relation among the three data bases. The tapes had D (dark 1inb), B (bright limb, sunlit feature or only codes for names and locations, the slips filled penumbra), U (umbra), or T (at terminator, consider- out by observers had no codes and neither did the ed as g). The "D/B" column on the left side of the publications of Russia or Czechoslovakia. A partial back of the IOTA/ILOC forms, 81 Feb Edition, should name/code list was found on one tape and a third no longer be used. tape provided location/codes. The name/code list was, however, old and many codes were not included. New IOTA/ILOC forms, 81 june Edition, have been pro- The occuitation tapes themselves (from RGO via USNO) duced, along with revised instructions, to include contained data from 1975 thru 1979. These showed the above changes. However, the 81 Feb Edition of dramatically that it indeed takes about four years the forms can and should be used until the supply of for the data to be properly submitted and collated them is exhausted, keeping in mind the above infor- 160 mation. It is important that the ILOC and IOTA/ILOC suspected secondary star, estimated to have occurred forms be used, rather than any other forms, use of half a second after the primary disappeared, is which will cause considerable delays in putting the given on the second line. The third line gives the data into computer-readable form for computing re- time observation of the graze began, with timing by siduals and for analysis. It is a major undertaking tape recording a mechanical clicker (equivalent to just to get the current system of keypunching and a tone generator) or voiced calls, and HWY shortwave reduction operational at the I.L.O.C., so we should time signals. The first event was a gradual disap- help them as much as possible by using the new forms pearance, with start and end of fade separately timed. The next graze event was a faint flash, en- I have been rather dismayed at the number of mis- tered on the sixth line, the last line shown. I takes on, and misunderstandings about, the new forms will describe how some of the information should be which observers have sent me so far. Be sure to completed below, referring to the example and point- read the instructions carefully. At least for the ing out some comon mistakes. first few forms you complete, I recormend using pen- cil, since it is much harder to correct forms writ- PLACE NAME: Give the name of the village, or other ten in ink. prominent landmark, closest to the point of obser- vation. Give the name of the city in which you As an example, I have partially completed a form for live only if you observed from home or if it is a hypothetical graze report reproduced above. This closer to your observation site than any other vil- can serve as a guide for correctly filling out the lage. forms. Two observers are included in the headincc, although only the first six timings by observer "a" ADDRESS: Give your complete address, including are listed. Several minutes before the graze, a street, post office box, or rural route number, total occultation disappearance of the star SAD city, state or province, postal code, and country. 098016 was timed with a stopwatch. It was suspected Also, include your name if you are not the only ob- ~ that the star disappeared in steps due to previously server listed on the back of the form, or if you unknown duplicity, so an uncertain timing of the are not the graze expedition leader specified on

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._.1 161

the back of the fom. some observers because it is exactly the opposite of the convention required for numbers, which must be TELESCOPES and POSITIONS, Type: A Newtonian reflec- written in the right-most columns, unless their pos- tor was used at station "a," so "N" is circled. At itions are fixed by decimal points. Be careful to station "b," a five-inch Celestron was used. Since follow the directions when completing these, and the it is a Schmidt-Cassegrain design, "C" has been cir- next few, columns; notice my examples. "E" has been cled, and the aperture and focal length converted to used for the event on line 2, "eye and ear," s.ince the nearest centimeter. "C" might also be used for the possible secondary disappearance was not specif- a Maksutov telescope, although, since the design is ically timed, but only estimated to have occurred slightly different, in this case, "0" could be cir- 055 after the primary disappeared. Code P should be cled and "Maksutov" written within the parentheses. used for any automatic (non-visual) method of re- cording occultation times, such as videotape as well Height: This should be in meters above sea level. as photoelectric. Multiply elevations in feet by 0.3048 to obtain val- ues in meters. Unless the site has been surveyed On the back of the form, the probable duplicity of accurately, the height should be given only to the SAD 098016 is noted in the coments for event number nearest whole meter. 2. The event position angle, cusp angle, and moon altitude are given, since these are useful for esti- Geodetic datum: This is not mean sea level, used mating the possible double star parameters. for vertical control. The geodetic datum is the horizontal control surveying system on which the At the bottom of the back of the form, "+" (waxing) map is based. FOr nearly all of North America, it or "-" (waning) Or "E" (lunar eclipse) should be is the North American Datum 1927 (NAD 27), while for given after the % sunlit, and "N" (north), "S"

\.~ most of Europe, it is the European Datum (ED, also (south), or "U" (umbra1 distance during eclipse) called Potsdam 1950). There should be a statement should be given after the cusp angle value in de- about the geodetic datum somewhere in the margin of grees. The Watts angle should be a value near the the map. If there is no such statement, the pub- center of the region of observed events, which may lisher of the topographic map should be contacted to be offset a degree or more (especially if the graze find out what it is. Note that the geodetic datum is near the terminator, with half the events not ob- usually does not have the same name as the rectangu- served because they were against sunlit features) lar grid system which is printed on many topographic from central graze. The latitude libration value maps. can also be taken from the predicted profile.

Star Name: Do not write "Z.C."; "R" is the code to There is no provision on the new form for the obser- be used for Z.C. stars (which have no prefixed ving condition code. For the time being, we plan to letter under the column "USNO REF NO" in the U.S. abandon it, but in case we later find it useful, for Naval Observatory total occultation predictions). example, for continuity with previously-reported R is used because Robertson published the currently- grazes, you might write "O.C.C." and give its value used Zodiacal Catalog in 1940. Whenever possible, in the upper left corner (above OBSERVERS and RECOR- avoid use of Durchmusterung (BD, SO, or CD) numbers DERS) of the back side of the form, or even for some since there is an ambiguity between BD and CD in the individual events in the comments section. -22° zone and there are not enough columns provided for CD numbers. The columns reserved for the dec- If you want to get some practice in completing the lination zone can be used for the star number if the forms, I have a large backlog of graze reports which catalog does not have declination zones and if the need to be transcribed to the new forms for process- number requires more than four digits, as is the ing by the ILOC. These include most of the 1978 and case for SAD and USNO "X" numbers. Since SAD num- 1979 graze reports written onto the old IOTA forms bers have up to six digits, a leading zero has been m which were never processed by H.M.N.A.O., and have written in column 18 for SAD 098016. been returned to me since they no longer have the manpower to do the job. Don Stockbauer and Robert Station, Tel, Obs, Rec (columns 24-34): Always Clyde have volunteered to do this work, but they leave these columns blank on graze reports since the could use some help in order to complete the job in ILOC needs to assign them. Instead, enter the ap- a reasonable amount of time. It is most important propriate telescope, observer, and recorder (if any) to get the data in machine-readable form so that re- letters in the T, 0, and R columns (SI, S2, and 53) duction profiles can be generated automatically and on the far right side of the form. For total occu1- comprehensive analyses can be performed. Transcrip- tations observed at your usual observation site, you tion to the new forms is the first necessary step in can put the USNO station code (such as, SA187) under this process. Station (columns 24-28), but columns 29-34 should be left blank until you are notified by ILOC of the OCCULTATION OF NUNKI BY VENUS, OUR LAST CHANCE numbers to be used in those columns, which will pro- TO SEE THE CENTRAL FLASH bably not be the same as the similar numbers as- signed by H.M.N.A.O. David kl. Dunham

Ph, phenomenon, column 35: Leave this blank if you The rare occultation of 2.1-magnitude Nunki (Z.C. enter 8 or 9 in the graze column G (73) or if you 2750 " SAD 187448 " ct Sagittarii) was discussed in use column 56 on the back for the gradual phenomena o.n. 2 (IQ) 122; the usual planetary occultation in- described above. formation about the event was included in the tables on pages 116 and 117 of the same issue. The rarity MR, method of recording, Columns 36 and 37: Leave of such an event is emphasized by G. P. Konnen and column 37 blank, not column 36, in case only one J. van Maanen in their article, "Planetary Occulta- code letter is used. I think that this has confused tions of Bright Stars," in j. Brit. astron. Assoc. 162

91 (2) ]48, 1981 February issue. They calculate East is favored, with the event occurring at high that occultations of first-magnitude stars by plan- altitude in a dark sky. In most parts of Europe, ets occur only once in every 190 years, On the aver- daylight, strong twilight, or low a1tituden'iayhinder age, whereas mutual planetary occultations occur observation. At the time of the occultation, the with a mean frequency of once every 40 years (we are sunset terminator crosses easternmost Holland, the now near the middle of an unusual 247-year period of German Federal Republic, the Adriatic Sea, and the no mutual planetary occultations). Only 3 first- southern Italian peninsula; this will be shown on a magnitude stars are available, since Aldebaran can regional map to be published in the next issue.. The not be occulted by any of the planets, at least not disappearance of Nunki behind Venus' dark limb in a until about 6000 A.D. (Venus), according to jean dark sky will be a spectacular once-in-a-lifetime Meeus in j.b.a.a. 70, p. 182 (1960). KOnnen and event for observers in central and southeastern Eur- van Maanen found that 23 stars brighter than magni- ope, the Middle East, eastern Africa, and the west- tude 3.5 can be occulted by the planets, and they ern Indian Ocean. list }4 occultations of these stars which happen be- tween 1900 and 2100. Only four of these occur dur- Observations of the occultation, especially photo- ing the next 70 years, all by Venus: Nunki on 1981 metric observations, made from several widely sepa- November 17; 2.9-mag. a Sagittarii on ]984 Nov. 19; rated locations will have special scientific value. 3.0-mag. it Sagittarii, 2035 Feb. 17; and 1.3-mag. Perhaps the most important result will be astromet- Regulus, 2044 Oct. 1. The 2044 occultation of Regu- ric. By accurately measuring the position of Venus lus will be a good event, similar to the one in 1959, with respect to the star, it should be possible to but few of us reading this will be able to travel to link accurate radio astrometric results (such as see it in a dark sky, which will occur around 120° from very long baseline interferometry) to the stel- east longitude. The central lines for the ]984 and lar fundamental FK4 system. In the radio reference 2035 events miss the Earth's surface. The southern frame, the orbit of Venus has been established ac- limit of the 1984 occultation crosses Canada. curately by tracking of the Pioneer Venus orbiter, " which has been linked with quasi-stellar radio Until 2044, only the occultation of Nunki on Tuesday, sources. Since Nunki is an FK4 star, the radio sys- 198) November 17, provides a central occultation of tem can be linked with the FK4 system, especially in a bright star visible under good conditions in areas right ascension, through astrometry determined from with a high probability of clear skies. The Middle [continued on next page]

VARIABLE ZODIACAL STARS LISTED IN THE SAD CATALOG, by David Herald Oh to 6h 6h to 12h 12h to jgh jgh to 24h Some time ago I prepared a comprehensive list of stars listed in the Gen- 109778 1.0 E 77963 0.6 L 119203 1.7 L 186237 1.2 L eral Catalogue of Varia- 109789 7.1 L 78024 1.4 L 138594 0.5 L 186452 1.2 L ble Stars, and its sup- 109934 7.7 L 78066 3.1 L 138666 5.8 L 161257 1.7 L plements, that can be 92853 1.0 L 78092 0.8 L 138725 1.1 L 161376 1.0 L occulted by the moon, 93115 3.8 L 78094 0.6 L 119433 0.8 L 186718 2.2 E and have a maximum mag- 76297 2.0 L 78098 1.4 L 139236 0.8 L 161444 1.2 L nitude of 10.6 at least. 76418 4.5 E 78120 0.6 E 139335 1.2 L 161502 0.6 E Eventually it is hoped 94036 0.6 L 78135 0.6 L 157936 1.3 E 161571 0.7 L to have the data includ- 76680 0.8 E 95862 0.8 L 139350 6.5 L 161754 0.5 L ed with the normal oc- 76788 2.0 L 79031 0.5 L ]39403 6.9 L ]87233 1.1 L cultation predictions, 94173 5.7 L 79070 8.0 L 158092 0.5 L 187294 0.9 E considerably improving 77084 0.6 E 96912 2.8 E 139594 1.1 L 161870 1.0 L the coverage of the pre- 94604 0.5 L 97083 0.6 L 158210 0.5 E 187349 0.8 L dicted data for variable 77299 1.8 L 79635 6.5 L 158369 0.8 E 161972 0.7 L stars which currently is 77330 1.0 E 79717 7.0 L 158394 5.1 L 187547 4.4 L very poor. In the in- 94779 0.7 L 97596? 0.9 E 158406 0.7 L 187624 0.7 L terim, and to avoid 77516 2.1 L 97631 1.0 L 15841] 0.5 L 162339 2.5 L problems of finding a 94837 0.5 L 80035 1.5 L 158473 0.9 L 162394 6.1 L star far fainter than 77730 7.8 L 97753 6.4 L 158607 0.7 L 162777 1.8 L predicted, the following 77756 1.9 L 97768 1.3 L 158665 0.6 E 163080 1.2 E tabulation gives the SAD 97854 0.7 E 158719 6.0 L 188715 0.5 E numbers of all ecliptic 97942 6.5 L 183401 5.5 L 188923 2. L variables (listed in the 80312 1.5 L 183578 1.0 E 163323 5.3 L SAD) which have a magni- 98075 2.6 E 159561 5.2 E 164750 2.0 L tude range of 0.5 or 98230 1.6 L 184232 1.4 E 164193 6.4 L more, together with the 80524 2.9 L 159918 0.8 L 164218 0.7 L magnitude range, and its 98266 1.1 L 184415 0.9 L 164320 1.3 E type; L for long-period, 80608 1.4 L 159981 5.7 L 164343 5.9 L etc., as distinct from 98769 6.9 L 184551 2.0 L 164507 1.1 L E, for eclipsing-type 99413 0.7 E 160116 0.8 E ]64558 0.6 E variables. The stars 118649? 0.6 E 184796 1.7 L 164829 0.6 E are listed in Right As- 138245 0.5 E 185020 1.0 L 146035 0.5 E cension order, rather 160299 6.6 L 146043 0.5 L than pure numeric order, 185643 0.7 L 165212 1.6 L to facilitate comparison 185745 1.0 E 146384 1.0 L with occu1tation predic- 185755 1.0 L 128374 0.8 L tions. 185899 0.5 L 146923 0.6 E 163

the occuitation. Nunki is much easier to observe cumference results in light equivalent to a 3.6- astrometrically than 13th-magnitude quasi-stellar magnitude star for each arc second around the limb. sources. The current uncertainties of a few tenths In practice, the flash will not be this bright due of an arc second between the two reference systems to a further attenuation caused by the ellipticity might be reduced to only 0?0], the accuracy claimed of the atmosphere. According to the data in Seiff from the analysis of the 1959 Regulus-Venus occulta- et al.'S tables, the flattening at 100 km is only tion observations by G. dc Vaucouleurs and D. Men- about 0.5 km. Elliot et al. show that the central ze1, Nature 188, p. 30 (1960 Oct. I), and Gordon flash maximum focus zone has a width 4 times the el- Taylor, Royal Observatory Bulletin No. 72 (1963). lipticity, which is 2 km, which would be covered in only 0511 of time and would be mag. 4.4 per arc Information about Venus' atmosphere can be derived second around the limb. It is doubtful that anybody from photometric occultation data. Although this will be so lucky to be that close to the central can not compete for accuracy with space probe data, line, but since the intensity drops off inversely data for several locations around the planet can be with distance from the center, the phenomenon should obtained nearly simultaneously at the time of the be visible over a considerable distance. At a dis- occultation. If Nunki is a close binary, the obser- tance of 67 km, which is ons at Venus, the inten- vations will reveal the duplicity, and the star's sity will be mag. 9.0 per arc second along the limb diameter might be measured for comparison with the and the duration will be 755. Since this is the ex- intensity interferometer results. pected maximum path prediction error, if there are 3 observers, it would be logical to station one at The most interesting aspect of this occultation will the center and the other two 67 km to the north and be the possibility of observing the central flash, south. In this case, the worst that could happen the focusing of Nunki's light by the entire circum- would be for the path to pass exactly between two

"~- ference of Venus' atmosphere when the star is di- of the observers, in which case, the distance would rectly behind the planet's center. The phenomenon be (t'075, giving a brightness of 8.3 mag. per arc probably will be visible, to some extent, from a second of limb for 3S8. If the miss distance were band about 150 km wide, which is about twice my es- O:'OS, the brightness would be mag. 7.8 per arc sec. timate of the uncertainty with which we can predict for 255. Of course, the more observers that can be the location of the central line. The observable deployed, the greater the chances that at least one ' path would be considerably narrower, and harder to of them will see a very bright central flash. Re- predict (substantially decreasing the probability member that the intensity will probably not be uni- of success for a given observer), for occultations form around the circumference of Venus, so that the of stars fainter than magnitude 3.5, and as noted intensity at some position angles on the dark side above, there are no possibilities for stars brighter will likely be several tenths of a magnitude bright- than this until 2044. The only observation of the er than the values quoted above. central flash to date was obtained by the Kuiper Airborne Observatory during the occultation of e The map shows the central occultation path, and off- Geminorum by Mars on ]976 April 8. Formulae for the set paths at 0!'2 intervals to 2?0 north and south, central flash phenomenon are given by J. Elliot et across eastern Africa computed from standard ephem- al. in Astrophys. j. 217 (2) 671, issue of 1977 Oct. eris and FK4 data. I have obtained an improved 15, where they discuss their Martian occultation re- ephemeris of Venus, based largely on the Pioneer sults. The central flash appears to the observer as Venus orbiter tracking data, from E. M. Standish of a ring of light around the planet at the time of the Jet Propulsion Laboratory. Also, Thomas E. central occultation. The intensity of the ring will Corbin, Transit Circle Division, U. S. Naval Obser- vary rapidly with time, and also with position angle vatory, has provided the latest accurately-reduced around the limb due to the ellipticity of the atmo- positions of Nunki from the Southern Reference Star spheric layer focusing the star's light. During the program and given me advice on applying various cor-

'~. occultation of Nunki, the central flash will probab- rections to reduce these to an inertial system some- ly be visible for less than 10 seconds. what better defined than even the FK4. Using all these data, I computed a new path, which is shown by From the 1959 occultation, dc Vaucoulears and Menze1 the line at about 0!'17 north. Shading extending determined Venus' occultation radius to be 6]65 km, "0!']5 from this line defines the most probable zone which is 55 km above the cloud tops. For the occul- of visibility of the central flash. The only land tation by Mars in 1976, Elliot et al. determined crossed by the path in reasonable darkness is in that the layer producing the central flash was about Ethiopia and northern Somalia. The chances are very 4 1/2 scale heights below the half-intensity inner- small that anyone farther west, in strong twilight sion and emersion layers. Applying this to the 1959 or daylight, will be able to see the central flash. data implies that the Venusian central flash should Perhaps the main uncertainty in the path results be produced by an atmospheric layer about 30 km from the uncertainty in the absolute right ascension above the cloud tops or 100 km above the solid sur- of Venus, which had to be determined mainly by opti- face of Venus. This layer is high enough that it cal transit data. The J.P.L. and Astronomical should be quite stable and free of dust, aerosols, Ephemeris right ascensions disagree by 0!'4. As and turbulence in amounts which could cause signifi- noted above, a major goal of the observations is to cant absorption or scattering. From the Pioneer resolve this discrepancy. The central flash should Venus probes, A. Seiff et al., j. Geophys. Res. 85 be a more precisely measureable phenomenon than (A13) 7903, special issue of 1980 Dec. 30, find the either imersion or emersion, which especially pressure at this level to be only 2 x 1q"4 bars. nighttime visual observers may find difficult to The maximum brightness of the central flash is lim- time due to their gradual nature over several sec- ited by Nunki's angular diameter, which subtends onds. Timings accurate to 055, which should be about 380 meters at Venus. This gives an enhance- achievable visually for the central flash, will give ment by a factor of 54 times Nunki's unocculted in- a determination accurate to 0!'02, while a QSj timing tensity, which when spread around Venus' 85!'7 cir- error would result in 0!'004. The central fiash will

G 164

also probe a deeper layer of Venus' atmosphere and suits are presented in tw'o tables in the same format will be produced by a large fraction of the circum- as those for the main list of 1981 planetary occul- ference, not just essentially single points probed tations in o.n. 2 (ID) 116-120; The occultation by by the disappearance and reappearance of Nunki. Mercury was not found by us, but rather by Steven Photometric observations of the central flash can Albers, who informed Sky and Telescope, which noti- probably yield data on extinction of the Venusian fied Dunham. We include it here for completeness. atmosphere, as the 1976 observations of the occul- tation by Mars did for that planet. Most events occur at relatively small elongations from the Sun, so that the durations are rather Hans-joachim Bode, director of the European section short, but most may occur in areas with potential of I.O.T.A., Bartold-knaust Str. 8, 3000 Hannover 91, observers. Three of the occultations occur at very German Federal Republic, and I are making plans for favorable elongations, and some of the others in- an expedition to Somalia to bracket the central volve rather bright stars. The first two events flash zone. We hope to use CCD arrays and sensitive will occur before this issue is distributed, but video equipment to try to record the phenomena with advance information about them has been sent to B-inch telescopes. Visual observations are also IOTA coordinators in the possible areas. Regional planned, and anyone else interested in joining us on maps and finder charts will be distributed, or pub- lished here, along with the maps and charts for the . shouldthis once-in-a-lifetimecontact either HansoccultationBode or meopportunityat P. 0. Box other 1981 events, as appropriate. Unfortunately, 488, Silver Spring, MD 20907, U.S.A.. We probably the plotter was not functioning well when some of will gather in Berbera, the largest city in northern the regional maps were drawn, putting bumps or small Somalia, where some Americans are stationed, and on waves on some curves drawn at certain angles. The the northern edge of the possible central flash bumps should be ignored; the smooth part of the line zone. We probably will deploy from there to other is correct. Sometimes, the problem was so bad that towns across the 140-km-wide path on Nov. 17, per- the lines appear almost as stair steps. You can _ haps with the help of a small rented airplane. I receive local circumstances for these additional ap- have obtained 1:250,000-scale maps of the area with pulses by sending a self-addressed stamped (for the help of Alan Fiala, U.S.N.O. The area is a des- those in the U.S.A.) envelope to Joseph Carroll, ert, and weather satellite photoes taken during the 4216 Queen's Way, Minnetonka, MN 55343; see p. 131 past 3 years show a high probability of clear skies. of the last issue. Notes about some of the events The infamous refugee camps are mostly in the south- are given below. ern part of Somalia, and mainly close to the border with Ethiopia, which we plan to avoid as much as Oct. 23: The nominal prediction was computed using possib1e;'weather prospects are slightly better an ephemeris generated from orbital elements deter- closer to the coast. Since logistic details have mined at the Institute of Theoretical Astronomy (I. yet to be worked out, it is hard to estimate costs TA.) in Leningrad. Orbital elements by Paul Her- get published in m.p.c. 4373 (1978) will probably now. Hans Bode informs me that round-trip air fare from Germany to Kenya is about $900, while discount give a better prediction, which is 0!'51 north of, fares (should be easy to get in mid-November) from and 3.4 minutes later than, the I.T.A. prediction the eastern U.S.A. to Germany and back are about used for my regional map and SOma's world map. Data $600. About November 8, there will be a national for the Herget element prediction are given in the meeting of German amateur astronomers which some tables. traveling to the occultation may wish to attend. If you don't want to travel to Somalia, you might con- Nov. 9, Mercury: SAD 139620'S magnitude is given sider other places where astronomical and weather incorrectly as 5.8 in the SAD catalog. At its true prospects for observing this rare occultation are magnitude of 9.], the occultation will be very dif- good, such as Saudi Arabia, Egypt, Israel, or, per- ficult to see due to the combination of low alti- haps, Turkey or Greece. Observations from more dif- tude and twilight. The possibility for seeing any- ferent latitudes will give better coverage. Gordon thing exists only for those in a narrow band a few Taylor is seeking others interested in traveling to degrees of longitude wide roughly along the eastern east Africa for the occultation combined with a hol- side of the Appalachian Mountains. iday tour; see the bottom of p. ]22 of o.n. 2 (ID), 1981 january, for details. Nov. 22: This occultation was not discovered by us, but was found by Gordon Taylor, who has already dis- MORE ASTEROIDAL OCCULTATIONS DURING 1981 tributed predictions for it. The star is the secondary of the double star A.D.S. 6308. The mag- Andrew Lowe and David It Dunham nitude of the primary is 8.7 and its spectral type is AS. The secondary, LO-magnitude fainter than Lowe has made a computer comparison of the SAD cata- the primary, is 4:'3 from the primary in p.a. 108°. log with asteroid ephemerides generated with Kepler- The primary will not be occulted, with its occulta- Ian formu1ae using the precision osculating orbital tion shadow missing the earth's surface by 760 km elements published in the Leningrad Ephemerides of (0!'51) over the Indian Ocean at 5h 45m U.T. in day- Minor Planets for 1981, Although planetary pertur- light. These calculations are based on an ephemeris bations were neglected, accurate calculations by computed from orbital elements by Paul Herget, which Dunham using numerically-integrated ephemerides probably give a better prediction than that derived showed Lowe's selection to be quite good. Of his from the orbital elements published in the Leningrad claimed occultations, all in fact were occultations, Ephemerides of Minor Planets for 1981 (E.M.P.81), and out of a similarly long list of close misses, which is very similar to Gordon Taylor's predic- one appu1se was actually an occultation. The tion. The e.m.p.81 ephemeris runs 3'.'88 west and 9% searches were restricted to minor planets with triad earlier than Herget's ephemeris, which produces diameters between 100 and 200 km which might not occultations of both components from the earth's have been included in Gordon Taylor's work. The re- surface. In this case, the path for the primary 165

star occultation will cross northern and western Eu- the Herget ephaneris is probably the better one, an rope, and northwestern Africa from 5h jgm U,T. to astrometric check is needed to be sure; some infor- 5h 38m, a path just a little east of the secondary mation about the discrepancy probably can be deter- star track produced by Herget's elements. The e.m. mined from analysis of observations of the asteroid p.81 path for the secondary star crosses the south- made during the past few years. Dunham plans to in- eastern U.S.A. , the Caribbean, and northwestern elude the results of such an analysis in the next South America from 5h 28m U.T. to 5h 44m. Although issue. The calculated diameter of the primary star 3 cl) qj 3 3 is 0.08 mi11iarcseconds = 116 m at Siegena's dis- o q)q)q)oq)o q) q) q) tance, so it would " ¶ —0oo~tn< la mm o=o =o = om dm 0_=m%±_ Lei CJmCm dc d= p- - take only 21 mil-. = ljj 3 x co 3 m g m = c em ¢u_x m eu e f = · <-_c')qooou)m"c")majmmcrblsj«¢n

0 ci) =mZ=ajc'juj=~wmmcjmcj m ~ lC'j i i m n 1_ 1c'jcyic\j~ * " ~ < «_ c»mcnm~ qc i t i i I iiiI tra11y occulted. O m mqoocvcjQocn¶ " qc" =0~aj pattern.. will be LLJ = cDLc)mmuDc'j- mC ·c ers. The magni" 'm VI = ·r (IQ C3 +M VD W m LO m m" . qjs- ?Q) +·cU · mC == =· = ·m4- ·g")· ~· co··uj ~· cn.,tude drop in case E :> ·m 3 ~ m cl) Ci = O Cj Ci o cj c3 of an occultation < m · -Q · _ V) V) i III .

(D · ·r-u «c.j e= cn S-= ~on C- m~ C'J m ·T of the . primary c.) or) l. >,~ s- q) cu < o' uj o c'j 4d m star will be 3.1. ·~ 4- S- O O.C.C Q) Q. = C'J C) — O C=) '~. S- · mC CO CD +J +J .Q X ~ CNS ~ 4- C m C · :3 X. -Q = G") O ·z · © m crs . = Cl o ·r- g.) m _ c) ~ c» ~ Nov. 23: The star " 3 +" cUCj)4" Q) V)2 S- 0 , . . . cu · s: ·~ · V) m q) pr- g) — cU <>< tarn = Z.C. 2750) mC " C"· = S- TJ e·· " (V C"· S. M O L) = " . ccscu ma:i= cn~a. ¢5qj e · ··m·m ¢5«3 4- c"^c^rcnocn~cn^m< lc^dlcjc"j¢ which remarkably ' = Q) ·m U X cU = ·~ U E m= ·m k.m G.) m - · · · · · · ·· ··· ·.... — cn ·m s- g ·m n ^·m = is occul ted by Vc- CJ .CI m QJ S- (I) S- V)+" m elS X- TJ :>,r· 4" mC (I) S- LLJ . ·~ ·mC4-+"OC~S-·m4- ·cm== nj 4- f— qj' nus only six days ~ V) N OmC·w+" qj S-CJQ-Qjcms)·d·m~_coµm·^~m^co~~C'JCrjC") ~ ye) crj _j_1_ cn©cnc^cj¢DLcj~¢Dcjc'j~ lc^dc\jw ~ that a south shift . = cin uj @i CT\C'J~OLS)OOOC"JLCJW ¢0^·±0 CD »s. Lcj<·mm~c'^nwc")c")mOC>CJOC>OOO0· · · ···· · - ...CJCJC>C3 ... ..D is needed for · the· = hd event to be VlS1- c.j cjajocnncocmncocno©N ·c»ajcom c3j m >- < b1e in the possi- c:) <1 r·^'jm"~ejm"^jm-cKl¢n0Lrj^j~cn<~Lcj qc LDLc)<-m"¢")mLc^c)c'j~^cnmmm"¢m - · ujlc)mooc")«)cmsjr·^vm£)~Nmer)oLD~ b1 e area. But at CJ· m¢\j^m'cnm"cm")cm£)c>m=c'j~·±ajmLA mtmM·~M·Lcj c>jc")Ln¢vujNc4 =o c>jc")«)mc'7omookDc")Qm"=Lnocnur)mc>jm-c")qm-c")cYIc")·d~·cnmu>jc")<¢ln~ least secondary Q) O <1C O ~ · ci Ls)cv^oc'jo\coco~c»ocnuj_~ e ~m·~~e)cnoNQoco_ajoc"^ocjco_~ occultations are I eg II ~ C\J~ I m 1C>JC'JC'J = mOC\j ICjCjCVOOCVN~Cj~ " c> I II II , i,, + ,, +++,, ,,, ,, ,, ,, possIble. The ap- Le) p- · m Lsjmor%mqomo\¢oc")Ln~©LA~Lr) oj rmx^ocDcmD<~©oc>jcDco~omo pulse occurs in q<= %^±No(s)~ujc>jq~co=c>j~c'jm=' "" · · · " ······ ·· · ·· = cv~~cvc'7Lnoujmcvc'j©mwLs)cy~m"< U'J <10 mcmnoco¢DLcjoe)ocmn~cvLc)cocom'oajoo0mc'jejLno m:E>j~ p- <-m~~cveoooLcj^Lcj~c'jo<~c'j0u> ' e '&jmojcm7bQommo\ckoo?^o=c'jcoajm^· ' · · ········· ····· cjx c3gu cv~r-~c")c")c·?c")Lnujm~jQ«Lc)c'ju")—mwcDcTbwLs^o=ajcm")mc")c»c>jmcn willtrometrypreventfromasthe- LO O , OO=OOCJCJCJCJO~OOOOOCJO u') =oj «j^r~r^"^r)cjncjcT\cmNaj_m·ocOLcjc'j~^mcvmou><^oo~oco~e)mcj q)| Northern Hemi-" S cna^r)c")m~^C>mcOq c»cdcdu)c»»=c»u)mLD^¢~ nitude· drop is· the F" " ···V-- · " · " · · " · · ·· · · · uj QC Le) <1 cn In cmncrlcvcmm_c'jcvcn~cvc>j~ m greatest I have LO = ~ Llj ^m ·cvr·^'^D^Lcj4MNr^DcDc")m¢ = cDc")^~u)co©^^ajm · ·· · · · · ·· · - ··· mC I cjm ·_OOQOOCDCM~DC>OO0 " E c")~m-~cvcn~cn~ejo~_cn~cnm · ·· · cj ··.·...... di cted occulta- = —— ~ ~~C———— I ——~—¢—— -J E O O D cjoooQoujocjoCjOoo on (s hd tion. The star < ·m4" GU ·mm elS (u ·rCO Q. m·m <^oLs)_mc')Lcj~~~mmo_~c")~_crj~mLc)o^D~cjrm=Lc)c'j~©~e)= probably can be m m e S- A ·~ >, C elS C i m~~~COC'jm~~~ · · _1 ljj ·m s.» (UE Cl)= ox ci= =+"cU-h'qj s-» q)g q)enc cO wCO cUm QC &e VI m

ujdc ~e doc")Lc)NcnLr^T·T'lc}cn©cnencvlncm>jmi F <1>~j· F- = c'j · cncr^ooqmj Crj c>j _ cv uj CV¢'jm·c"^c)~Lc)c>Qc'^cjou>~cncncoLjn^m cnej Crj ej eg C\j ~ c>j Nunki· will· be 41' CO i— CO F- =s £%gg?#€m=tmbcee## 2& g6ggb"##=%bbcb#e#e '°"h of Venus in mm<

THE GRAZE OF IOTA AQUARII near the moon's south pole.

David Id. Dunham This rare grazing eclipse, technically called a "grazing occultation," or simply a "graze," can be A grazing occultation of the 4th-magnitude star Iota seen with a small telescope or even a pair of binoc- Aquarii (Z.C. 3237) took place on U.T. 1980 November ulars. If binoculars are used, they should be 16. It was the most favorable graze to pass near mounted on a camera tripod or steadily held against several large cities along the east coast of the USA something, such as a fence post. during the past few years. The time was convenient and the path passed right over Washington, DC. Of A graze of a star bright enough to see with binocu- course, it rained or was cloudy along the entire lars occurs at a particular place only about once in path; only one observer in a Rhode Island expedition every 50 years, while one may have seen the first disappearance in a break in such event visible some- the clouds (he was unsure). Nevertheless, the graze where from the Washington generated much interest, and was favorable enough metropolitan area might that some interest might be generated among the gen- occur about every ten eral public. I prepared the paper, printed below, years. The graze will be 0 and sent copies to the local major daily newspapers, visible only within the 2¥ and to amateurs in other cities suggesting that they mile wide band shown on make local modifications and do the same. You might the map. South of the 1 consider preparing a similar article when a very southern line on the map, favorable graze next passes over your metropolitan the moon will miss Iota area. The Washington newspapers did not publish Aquarii altogether, with The diagram above anything about the event; their science writers were no eclipse occurring. shows the moon as it in California for the Voyager Saturn flyby that North of the northern will appear at the week. Paul Teicher did manage to get a shortened line, a short "ordinary" time of the graze of version of the paper published in a Long Island, NY, eclipse of the star can be Iota Aquarii on Satur- newspaper. It might also be useful to contact the seen. There, Iota Aquarii day evening, Nov. 15. electronic media. I did this locally so late that will disappear at about The darker areas on the long-range weather forecast already was pessi- 8:35 p.m., and will not the moon's bright side mistic, but radio station WTOP did interview me on reappear until several are the maria, ancient the air by telephone. Since that station was the minutes later. seas of frozen lava one we selected for the secondary time reference, which form "the man in "" the announcer asked me about that, which gave me the The moon will be near the moon" figure at opportunity to explain how members of the public first quarter, with 54% full moon. The long could make useful observations. The map showing the of its apparent disk ii- arrow shows the motion path, traced from a 1:250,000-sca1e topographic map 1uminated by the sun. The of the star relative plot, is not reproduced here. On 1981 january 14- rest of the disk will be to the moon as seen by 15, a graze of Z.C. 444 followed a nearly identical faintly lit by "earth- observers in the pre- path across the Washington area, but we did not pub- shine," which is sunlight dieted graze zone licize it since binoculars would not be sufficient reflected from the earth. shown on the map. The to see it. In spite of a pessimistic weather fore- If you know where to look, star at the base (up- cast, which discouraged many, the skies cleared a Iota Aquarii can be found per left side) of the few hours before the graze, which was timed by sev- easily with the unaided long arrow shows Iota eral observers, some of whom successfully used WTOP eye from a location with a Aquarii's location a for a secondary time reference (I made the wop - relatively dark sky. Dur- half hour before the IdldV master tape). ing a graze, the moon pro- graze. The short ar- vides an easy reference row indicates where Moon to Graze Bright Star in for finding the star, but the graze will occur. Washington Saturday Night, Nov. 15 also produces so much glare that at least binoculars are needed to see the About 8:40 p.m. Saturday evening, November 15th, star. those living in a narrow zone passing across the Washington area may be able to see the bright star The graze of Iota Aquarii will occur entirely on the Iota Aquarii (Iota in the constellation Aquarius) dark side a short distance from the moon's southern disappear and flash back into view several times as cusp (normally called a "horn" when the moon is it appears to skip along a rugged mountain range crescent). 167

The moon, which will be high above the southwestern not accurate enough for this type of observation, horizon, will seem to drift from right to left in but the time available from the U. S. Naval Observa- relation to the stars of Aquarius. Hence, relative tory, phone area 202, 254-4950, is accurate enough. to the moon, Iota will seem to move from left to right, as shown in the chart. The graze will be In addition, the place of observation must be known about five minutes in duration, beginning just be- to an accuracy of ten feet with respect to nearby fore 8:41 p.m. rQad intersections, railroad tracks, creeks, or large buildings. If you do make a successful re- If the successive disappearances and reappearances cording, telephone David Dunham at 585-0989 or write of a star during a graze are timed to an accuracy of to him at P.0. Box 488, Silver Spring, MD 20907 to one second or better by observers at several loca- report the necessary details of the observation. tions across the predicted path, the moon's position in relation to the star can be measured to high ac- If you do not live in the predicted zone, but are curacy. These data are valuable for studying the interested in seeing the graze, you might visit a shape and motion of the moon. Lasers are used to friend who does live in the zone, or just try to ob- measure the moon's distance precisely, but observa- serve from any accurately identifiable position tions of grazes are needed to examine the small within the zone. Members of the local astronomy north-and-south variations in the moon's motion and club, the National Capital Astronomers, plan an ex- to orient the lunar orbit relative to the stars. pedition to observe the graze from several locations The two types of observation complement each other across the path. If you want more information about to give a better description of the moOn's orbit and the graze, or want to join our expedition, call Da- of the basic stellar reference system used by as- vid Dunham at 585-0989 or at 589-1545, ext. 358. tronomers. Graze observations are analyzed at the U.S. Naval Observatory, Washington, and at the Royal When the light of Iota Aquarii is spread out into ~. Greenwich Observatory in England [Ed: currently, its different colors with a spectroscope, evidence substitute ILOC for RGO]. for two stars very close to each other is revealed. During the graze, the second star, which has never The lunar profile can be approximately predicted us- before been directly observed by itself, might be ing photographs of the moon which have been measured seen briefly after a disappearance or just before carefully at the U. S. Naval Observatoig. But the the reappearance of the main star. Or the second profile can be traced more accurate1y"with extensive star may simply cause some of the disappearances or graze observations than it can be dCduced from pho- reappearances to appear gradual, lasting a few or tographs. several tenths of a second, rather than instantane- ous, as they normally appear. A small telescope may Recently, solar physicists have postulated small be needed to observe such "step" Or "gradual" variations in the sun's diameter which can influence events, but if they are seen, try to note both the the earth's climate. Astronomers have found that beginning and the end of each event in your record- careful observations of total solar eclipses provide ing. a powerful method for monitoring the solar diameter. But in order to use these solar eclipse observa- The path for the Iota Aquarii graze extends across tions, a good knowledge of the lunar profile is the United States from southern Texas to Massachu- needed. Grazes of stars help provide the details of setts. It passes near Lafayette, LA; north of At- the lunar profile. lanta, GA; near Roanoke and Charlottesville, VA; south of Wilmington, DE, and Camden, Nj; over Long Anyone within the graze zone who has a tape recorder Island, NY; over New London and Groton, CT; south of and binoculars could make observations of scientific Providence, RI; and north of Plymouth, MA. Other value. The more observers who record a graze from expeditions by amateur astronomers are planned in different locations spread across the zone, the more most of these areas; if the weather cooperates, it m. accurately the lunar profile is traced. To observe, could become the best-observed graze yet. place the recorder close to where you watch the graze, so that your voice can be recorded. Fresh VIDEO RECORD OF MULTIPLE EVENTS DURING GRAZING batteries should be used. Small tape recorders need OCCULTATION OF 0 CANCRI REVEALS DIFFRACTION to be protected from the cold, to prevent the motor PHENOMENA grease from freezing. For example, the machine can be kept under your coat, perhaps hung from the neck David Id. Dunham, Alan D. Fiala, and joan B. Dunham with a loop of twine. Start recording about 8:38 p.m. and be sure that you have at least ten minutes In spite of a pessimistic weather forecast, clear of tape. Each time the star disappears, call out skies prevailed near Conowingo Dam, Maryland, on UT "off" or "on," respectively. If the star is 1981 May 10 (May 9 local date, Astronomy Day), per- eclipsed briefly by a small hill, so that it reap- mitting observation of the graze of 4.2-magnitude pears imediately after it disappears, we call the 0 Cancri (Asce11us Australis = Z.C. 1310) from 16 of event a "blink." Similarly, a "flash" occurs if the 18 stations spread over a distance of 2.4 miles per- star appears momentarily in a lunar valley. Also, pendicular to the predicted limit. A miss occurred you should record WTOP at 1500 kilohertz using an AM at the two northernmost stations, but multiple e- radio nearby (a car radio could be used). Check be- vents were seen at nearly all of the other stations. forehand to be sure that both your voice and WTOP Analysis of the data is still in progress for the are clearly recorded. WTOP is used to provide a graze, important because the latitude Vibration was time reference for your observations; if a short- +0?07, well within the range for solar eclipses. wave radio is available, it would be better to use WldV at 10.0 megahertz. We will make a master re- At one of the stations, we attached an R.C.A. 12- cording of ldTOP along with ldWV to calibrate every- volt TC 2055 Ultracon low light level video camera one's WTOP recording. Ordinary telephone time is to an B-inch Celestron loaned to us by Mark True- 168 blood. The camera was small enough (2 pounds) so The advent of automatic recording methods does not that no special counterbalancing was needed; this decrease the need for, or value of, visual observa- was even the case when we tested the unit with a 5- tion of grazing occultations. To be sure, most of inch Celestron a few nights before the graze. The the information about the 0 Cancri graze profile video equipment was loaned to the U. S. Naval Ob- will be derived from the data of the 15 visual ob- servatory by Robert Flory, a senior engineer at servers. Visual timing accuracies for grazes are R.C.A.'S David Sarnoff Laboratory in Princeton, NJ, more than adequate for our studies to improve the originally to record the annular eclipse in Tasmania lunar profile, for solar eclipse analyses, and for last February, prevented by clouds. The camera out- astrometric studies; continuing substantial predic- put was fed to a half-inch Panasonic portable VHS tion errors constantly reaffirm this. Automatic video recorder-player. There was not enough time to records of grazes will be useful for assessing the secure a source of AC power for the telescope drive; smoothness of the lunar limb at the scale of Fresnel the video equipment was all battery-powered. We diffraction, since a perfectly smooth lunar limb is found that the star drifted across the monitor usually assumed for analysis of photoelectric total screen in 50 seconds, so that manual adjustments, occultation data. Also, automatic records of grazes during which the star remained in view, were made of close double stars, with two or more contacts ob- slightly more often. served, can give separations and position angles, not just projected separations, to considerably bet- Playback of the videotape after the graze showed 14 ter accuracy than visual observation. For individu- events (occultations by seven lunar features) in a als or societies who would be interested in record- period of 62 seconds, luckily one of the highest ing grazes and/or total occultations (especially numbers in the expedition. After helping with the reappearances) with video equipment, a camera like setting up of the equipment, Joan moved to a site the one we used can be purchased from a video equip- approximately 70 feet to the north (measured per- ment store for about $1200. A video recorder and pendicular to the limit), where she timed ten events other needed accessories typically cost a similar visually; the shadows of the tops of two lunar hills amount. The TC 2055 Ultracon has a light range of passed between the stations. David timed eight e- 1:660,000 and a fast response which minimizes the vents at his site 500 feet farther north. His first image decay time. disappearance was gradual, lasting 1.4 seconds, fol- lowed a few seconds later by a faint flash of about As far as I know, this was the first time that mul- seventh magnitude. The graze was very easy to see tiple events were recorded during a graze with video since the 41%-sunlit waxing moon was at an altitude equipment. In 1973, Joan photographed grazes of of 47" and the cusp angle of central graze was 4°N. Alcyone (t) Tauri = Z.C. 552, mag. 3.0) and Tejat (µ Geminorum = Z.C. 976, mag. 3.2) with 35-mm recording Playback of the videotape at tenth speed (three film pushed to ASA 4000. A motorized back for the frames per second) shows that the recorded events camera, attached to a 60-im refractor, permitted are gradual, some lasting 15 frames or more with un- 1/4-second exposures at 1/2-second intervals. Four dulations as the distance from the star to the edge and six events, respectively, were photographed, but of the moon varies. For each of these frames, we the timing was not as accurate as could be done vis- plan to estimate the brightness of the star relative ually. Video records have been made of three grazes to its unocculted intensity, and from that compute of first-magnitude stars, but in each case, only one the distance to the lunar limb from the calculated disappearance and one reappearance occurred. The Fresnel diffraction pattern. In this way, we can first was on 1976 August 29, when Spica was recorded trace the limb at 30-meter intervals, the amount of with a 48-inch Air Force satellite tracking tele- lunar motion between frames. Relative times will be scope at Malabar, FL. The site was several miles accurate to the frame interval of 1/30 second. We north of the southern limit, so it is not surprising did not make any proviSion for absolute timing other that only one R-minute occultation occurred. than recording MAY on the audio channel of thf video Harold Povenmire reported that Spica's individual tape, from which we can determine U.T.C. to 0.1. hie components were seen due to the high time resolu- _ are searching for a practical means for obtaining tion; the observation was mentioned in o.n. i (ID) U.T.C. to an accuracy comparable to the frame inter- 94. Portable equipment was used for the other two val, although such accuracy is not needed for graze events, Regulus on 1980 June 18 in New Orleans, LA, observations considering the present state of the o.n. 2 (g) 101, and Aldebaran on 1981 February 12 in art. the German Federal Republic, cormunicated by Hans Bode. Dr. j. Donunanget has been determining accur- We plan to makC a movie copy of the video record for ate times of total occu1tations, including rather showing at meetings. The equipment proved to be faint stars, with video equipment at the Belgian very practical for field use. It should be possible Royal Observatory during the last few years. He to record grazes (or total occultations, lunar or notes that the video method is the only one now cap- asteroidal) of seventh-magnitude, or fainter, stars able of recording reappearances and disappearances using a 14-inch Celestron, one of which is owned by equally. Not knowing the exact position of emer- our area astronomical society, the National Capital sion causes longer reaction times for visual obser- Astronomers. For recording total occultations, pho- vers, while photoelectric observers need larger dia- toelectric equipment, such as that designed for ama- phragms for reappearances. Domanget has published teur use by the University of Texas mentioned on p. an article about his method, "Observation des occul- 155, will give better time resolution. But video tations a l'aide dune camCra dc tC1Cvision," in equipment is much more practical for recording graz- Communications of the Belgian Royal Observatory, es and reappearances, since accurate tracking is not Series B, No. 104 (1978), and in Ciel et Terre 94 needed. The automatic timing of reappearances, (5). 1978. The variations, or "undulations" noted eliminating the uncertain estimates of personal above in our 0 Cancri record, are too large to be equations, could be especially valuable since few of caused by the diffraction pattern fringes. Probably these events are timed photoelectrically. they are caused by small lunar hills near the point 169

of contact, which cause the distance to vary on the IL, and 501,771-0978 in Little Rock, AR. In the steep part (major drop) of the diffraction curve. case of an unusually favorable event, as indicated by the astrometry, we will try to have a message ASTEROIDAL OCCULTATION UPDATES broadcast on HblV. Since Sky and Telescope is pub- lished more frequently than o.n., asteroidal occul- David IQ. Dunham tation news and finder charts often appear there first, so be sure to check Sky and Telescope. Finder charts and regional maps are published else- where in this issue for several potentially favora- I recently have made additions to my computer pro- ble asteroidal occultations for North Americans. grams so that most of the labels on my regional This material for the occultation by (IB) Melpomene planetary occultation maps now are written automati- on August 7 was sent to photoelectric observers in cally by the plotter. This eliminates the need for the western U.S.A. since the small magnitude drop me to add most of the labels manually, but sometimes virtually precludes visual observation and this makes the labels hard to read, when they are printed issue will be too late for that event. World maps on top of each other, or over crowded national for all asteroidal occultations through 1981 Oct. 5 boundary areas. I check the maps to see whether were published in the last issue. difficult area can be figured out from adjacent la- bels, and sometimes add manual labels for clarity. For the August 7th event, Arnold Klemola 9btained a A minor error, which soon will be corrected, caused plate connecting the objects on june 30 at Lick Ob- many of the labels on the charts in this issue to be servatory. This shows a CL'42 north shift with the plotted at a slight tilt with respect to the curves event 21!12 earlier than the nominal prediction, in- along which they were supposed to be plotted. dicating a path crossing southwestern British CoIum- The occultation by (48) Doris on March 19 seemed to ." bia,parts theof NewHawaiianSouth WalesIslands,andandVictoria.the southeasternFurther as be relatively unfavorable, but as far as I know, it trometry is planned to refine the prediction. Long- was the only asteroidal occultation to be observed, focal-length direct photographs of Melpomene, simi- from Washington and British Columbia, since the last lar to the ones of (9) Metis taken by Chinese astro- issue was distributed. The path was accurately pre- nomers discussed in the last issue, might show the dicted from measurements of a plate taken the night satellite suspected from the 1978 December 11 secon- before with the 6I-inch U. S. Naval Observatory tel- dary extinction recorded at Fernbank Science Center escope at Flagstaff, AZ, with reductions using faint in Atlanta, GA. reference stars tied to Perth 70 positions with a plate taken earlier at Lick Observatory by Klemola. Klemola will also attempt at least preliminary as- More information about this event, and other aster- trometry for the occultation by (70) Panopaea on oidal occultation attempts, will be published in the Aug. 26, and perhaps also (89) Julia on Aug. 12. next issue. The discovery of a probable third sat- Astrometrists in the eastern U.S.A. will give pri- ellite of Neptune during the May 24th appulse with Ority to the occu1tations by julia; (105) Artemis on KMN 29, with confirming photoelectric observations Aug. 27; (230) Athamantis on Aug. 15 (moonlight will by University of Arizona astronomers at the Catalina hinder, and possibly prevent, last-minute astrome- and Mt. Lennon Observatories, will also be described try); and (409) Asµsia on Aug. 20, in that order. in the next issue. Gordon Taylor plans astrometry at the Royal Green- wich Observatory for all events potentially visible On p. 152 of the last issue, for the occultation by from Europe. Metis on June 14, the label above the dashed line should be "Z.C.", not "AGK3". A special notice was The Asteroid Intercept Radio Network has been dis- sent to about 60 observers in the possible area of banded due primarily to the infrequency of events visibility, and astrometry by Klemola indicated only and partly to lack of interest of amateur astrono- a small north shift. The only observations received " mers in this method of shift dissemination in most so far are negative ones from the Purple Mountain areas. For future events, we will rely mainly on and Yunnan Observatories in China, and from Dushanbe the recorded message phone numbers used for the ill- in the southern U.S.S.R., all south of the path in- fated June 5th occu1tation, 312,259-2376 in Chicago, dicated by Klemola's astrometry.

Note added 1981 july 29 (addition to the "Using the The figures on IOTA/ILOC Occultation Report Forms" article, p. 159) this and the following pages Don Stockbauer points out that the foms still con- are an exten- -.j':j5t5ga'y¢?:.?y, tain no explicit' µjvisi0ns for "resumed observing, sion of the status changed" for the case where, during the "Planetary Oc- graze, the star disappears or reappears during an cultation Pre- . 6[:):"::.'i,/':'"g:Z. i: i '\, ,\ E':i.,,, Pi interruption of observation. For now, in this situ- dictions" arti- ation, enter "8" in the graze column 73, and state cle. The world in the coments that the star disappeared or reap- --'"g:'")'"i,,'),,/!):)!,.-):,',)),,':)!~ maps are pro- peared while not observing. Also, do this in the duced by Mitsu- case where the star already has disappeared by the ru SOma. The time that effective observation has begun, as is of- regional maps ten the case with waning-phase grazes when the first are produced by disappearance is on the sunlit limb. I have asked David Dunham. the ILOC whether a special graze column 73 code can Finder charts be designated for this purpose, which would elimin- are prepared by 'Ij)|)'"""""""'" ate the need for a connent, and will report their several volun- response in a future issue, teers. SAD 99321 by Aemilia 1981 jun 22 ]70

|S8; 8 12 (EB) J.LIA. SAD 58 135

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_- .__ 19Bi 8 2CJ ('¶29) AS'ASU SAD lC6373 70j 0 , DIAPERA 194 KM m (J:'!6 !E~c +="',,4:~jZZ, mS N q \ 7_4— " " - I 65 , _ "" I °¶C 7 I 0-3 " I ' , " % I j " I 6"· ' 4" \ ( t SAD 143526 by Athamantis'81 Aug 15 M,-r\ , , / N )icjjj/""" -.- :.zy's'": "K

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1981 8 13 (OIl) AMAMANT15 SAD 14=26 Diapeter 116 km = cjt'n 63 I "

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1981 9 20 (]4) IRE:E SAD 19]415 ·37°, Q a . ,ti ;yi . k,«\!h" '(: DIA'ETER 155 m - CJ:'] G , , Q q QO 0 0 t: d "» · e·r' b r";t, ' " ^,,. o g o i ' " qd " 7H +& . Cj O 0 mp W 0 , I ,360_ 0 "' "m' 9 , f -or . 58¶188,=o. 'i ."m OO Q i"/. . ° . "j-:?"l., n W ,,lS ;·¢\,: ! 3- 4' e ° . O"Q" ° 0 (I) ° i i." " ° °J ;7g"w' g' '"· '"^4 rz ,,,?: , ¶§ @ O; " ' ', . . ". '.% ":; :·' : ;:j'" i · ' :r0"':":.":,:y } '5p:" "CI ".1,. " . Iy ,;µ0 O % O " B . J ) " " ' ' " '" T ' / ,/ /( / , 0" . 0 i . b t q G 8 oq"(S I /",0 . ·- I. " . P C ° qC ° . ",' q ' ,§,OC g I 1, Li '"'" '· I "—S a" " Y O e G I +,Z!7 " " , - n " —

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Lj\SITLDE Nunki by Venus 1981 Nov 17

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