i Occuttau'mgNewsteuer

Volume IV, Number 1 July, 1986 Twelfth Anniversary Issue Occultation Newsletter is published by the International Occultation Timing Association. Editor and compos- itor: H. F. DaBo11; 6 N 106 WhiteOak Lane; St. Charles, IL 60174; U.S.A. Please send editorial matters, new and renewal memberships and subscriptions, back issue requests, address changes, graze prediction requests, reimbursement requests, special requests, and other IOTA business, but not observation reports, to the above.

FROM THE PUBLISHER IOTA NEWS

This is the third issue of 1986. It is the first David Id. Dunham issue of volume 4. As o.n. 3 (16) was being assembled, it became clear that it would be much larger than most recent is- When renewing, please give your name and address exactly as they ap- pear on your mailing label, so that we can locate your file; if the sues. This, coupled with the fact that we are about label should be revfsed, tel) us how it should be changed. three months behind our overall publication sched- ule, made DaBo11 and me decide that this would be a If you wish, you may use your VISA or MasterCard for payments to IOTA; include the account number, the expiration date, and your signature. good time to split the issue in two. lde expect the Card users must pay the full prices. If paying by cash, check, Or next issues to be smaller. The disadvantage of do- money order, please pay only the discount prices. ing this now is that we also have to split volumes. Full Discount price price This is the first issue of Volume 4, starting the IOTA membership dues (incl. o.n. and any supplements) thirteenth year of o.n. publication. for U.S.A., Canada, and Mexico $11.46 $11.00 for all others (to cover higher postage costs) 16.67 16.00 Those whose subscriptions expire with o.n. 3 (16) Occultatlon N~gletter subscrfptionj (I year " 4 issues) are being sent this issue anyway, to prevent the by surface mail for U.S.A., Canada, and Nexico2 7.28 7.00 need to send it when subscription is renewed. Sub- for all others 7.12 6.84 scribers and IOTA members are reminded that all by Ur (AO) maiP payments and questions about subscription and renew- for area "A"' 8.91 8.56 for area "g"S 10.32 9.92 al should be sent to the address in the masthead. for all other countries 11.75 11.28 Anything sent to the old address in Columbus, OH, can result in long delays, including lapse of serv- Back issues of o.n. by surface mail q.n. I (I) thru o.n. 2 (13) each ).04 1.00 ice. o.n. 2 (14) thru o.n. 3 (131, each 1.46 1.40 o.n. 3 (14) and later issues, each 1.82 1.75 Normally, in the first issue of a volume, we publish Back issues of o.n. by air (AO) maiP explanations of the tables of grazing occultation o.n. : {14]I) thruthruo.n.o.n. 2 3 (73),(13), eacheach 1.511.93 1.451.85 - observations, and of the planetary/asteroida1 pre- o.n. 3 (14 and later issues, each 2.29 2.20 (There are 16 issues per volume, all still available) diction tables, maps, and finder charts. However, Don Stockbauer published an explanation of the graze Although they are avaf)ab1e to IOTA members wIthout observation table only three issues ago, in o.n. 3 charge, non-members must pay for the following items: Local circumstance (asteroidal appulse) predictions (13), 273, so we will probably wait until the first (entire current list for your area) 1.04 1.00 issue of 1987 before repeating it. Graze limit and profile prediction (each graze) 1.56 1.50 Papers explaining the use of the predictions 2.60 2.50 The explanation of planetary/asteroidal occultation Supplements for South America will be available at extra cost through predictions is given in a separate article, although Ignacio Ferrfn (Apartado 700; Merida 5101-A; Venezuela), for Europe the only new events published here are the few by through Roland Bonfnsegna (Rue dc Marfembourg. 33; 8-638) DOURBES; Belgium), for southern Africa, through M. D. Overbeek (Box 212; Eden- (46) Hestia, for which the stellar data are incom- vale 1610; Republic of South Africa), for Australia and New Zealand, plete. Edwin Coffin's comprehensive predictions and through Graham Blow (P. 0, Box 2241; Wel11ngton; New Zealand), for Ja- charts have changed coverage for these events, as pan,Jim Stamthmu1Routeh Toshio3, HimseBox 109;(1-)3London,ShlmomarukoKV 40741;l-chome;U.S.A.)Ota-ku,by surfaceTokyo )46, japan . Supjlements for all other areas will be available from discussed in o.n. 3 (14), p. 301 and 303. In this issue, we include complete finder charts only for mat) at the low price of 1.23 1.18 or by air (AO) mall at 2.04 1.96 those events for which Goffin did not send us infor- mation. Detailed one-degree Astrographic Catalog Observers from Europe and the Brftish Isles should join IOTA/ES, send- (A.C.) charts only are published for several of Gof- ing DM 50.-- to Hans-j. Bode, Bartold-knaust Str. 8, 3000 Hannover 91, German Federal Republic. Full nmbership in IOWES Includes the sup- fin's events in this issue. The corresponding AGK3- plement for European observers. based and fifteen-degree field finder charts by Gof- fin (the latter annotated by others) have been pub- i Single Issue avaflable at k of price shown. 2 Price Includes any supplwents for North American observers. lished in o.n. 3 (14) Supplement for North American 3 Not available for U.S.A., Canada, or Mexico. Observers. An addition to this supplement was dis- ' Area "A" includes Central America, St. Pierre and Miquelon, Carib- tributed with o.n. 3 (IS) in April. bean Islands, Bahamas, Bermuda, Colombia, and Venezuela. If desired, area "A" observers may order the supplement for North American observ- , ers by surface mail @ 1.23 1.18 (3123) Dunham (see o.n. 3 (16), 351) is 17th magni- or by afr (AO) mail @ 1.56 1.50 tude at mean opposition distance, near the center of 5 Area "B" fncludes the rest of South America, Mediterranean Africa, and Europe (except Estonia, Latvia, Lithuania, and U.S.S.R.). the main asteroid belt. The estimated diameter is

1 2

13 km. The orbital inclination is only 2" to the ecliptic, and the perihelion dis- tance is 2.13 A.U. It is now near conjunction with the Sun and will have a favora- ble opposition early in 1987. Since the May 10th IOTA meeting (see p. 339 of the last issue), Derald Nye has suc- ceeded in developing the software for his IBM PC so that he now can take over the m~c")werjN< work that Berton Stevens has been doing in keeping IOTA'S computerized records. We aou^cmad sincerely thank Bert for the important work he has performed for IOTA for such an njcvr'jQjm ^0oajcomwu"j OCCULTATIONS OF ASTROGRAPHIC CATALOG STARS BY (46) HESTIA njw m¢~¶,D~~LD 0coumsjo^w David W. Dunham WCVC4¢VmmN Ooooo=o000 0 0 0 The asteroid (46) Hestia has become of special interest recently, since it has been ©~NN~tocn ~^jc'jNc'jcnw found to be the best asteroidal target for the CRAF (Comet Rendezvous and Asteroid <'e·a·w'q'«w Flyby) spacecraft mission proposed by the Jet Propulsion Laboratory (JPL). Remark- mOmmc\jGrLn ably, the same asteroid is also the best asteroidal target, and easiest to reach, f2~mmmm for a multi-comet flyby mission proposed by R. Farquhar of Goddard Space Flight Cen- bOOdOOO ter, even though the spacecraft trajectory and Hestia encounter time and speed are :3= uj "- completely different from those envisioned by CRAF. Although the planned Hestia m~u7u')—O— m m OLD «; flyby dates are a decade away, now is a good time to start more detailed studies of qj cl} Q) O h m 0 this object, since we are approaching a favorable northern-declination opposition in IIIIItI cnmDAY ,P,A R,A, REC. occultations by Hestia during the next several years. This search revealed six oc- EL M 0 N (46) HESTIA MOTION A P R E T cultations from june 14 to july 6 that might be observed. I distributed a special notice about these events to IOTA coordinators in the possible areas, which included southern South America, Mexico, and southeastern Australia.

On june }4th, nine days after I distributed the notice, I received Minor Planet Cir- cular 10,752, dated May 23rd, that contained an updated orbit for Hestia determined by Don Yeomans, JPL, using 149 observations made during 33 oppositions from 1912 to 1985. Fortunately, the new orbit passed only 0?6 north of Herget's orbit, and just under a minute ahead of it, during June 14 — July 6.

A table given in the usual o.n. fomat is included here, with several columns of constant or unavailable information deleted. FOr example, since spectral types are not available for these A.C. stars, their angular diameters, and associated parame-

ters, can not be computed. Yeomans' new elements were used to compute the data in h m O S the table. Mitsuru SOma used Herget's data to prepare his maps; I have drawn a sol- id line on each of them to indicate the path calculated with Yeomans' elements. The "possible area" for the listed events is quite uncertain due to possibly larger- than-usual errors in the stellar positions. Although the star positions could be improved from existing plates, the relatively small elongation from the sun will hinder astrometry for Hestia before mid-july. The finder charts for the events pub- T A R OCCULTATION lished here have been compared with Papadopoulos' True Visual Magnitude Atlas (T.V.M.A.).

Mitsuru SOma used ephemeris data supplied by me that were computed using Herget's cno¢'jcnr~=cn orbital elements for Hestia. The time differences, in the sense Yeomans — Herget, 00 0 B pg0

Ka.(1950)dec. A!!! Our, qf E possible area ¢QO'u*«C\jCO^ that should be applied to the times shown on SOma's world maps are given in the ta- «cvmcnuj ¢^cxjm'D~Ln······· mO~OmCjC> m mine; he used Herget's formal elements m m m july 25 -1.0 published in M.P.C. 4363, and AGK3 data = comcncn~couj F—< cj~~~tr>cvN Aug. 23 -1.8 for the stars, which are certainly bet- uj 00p·B 00 =·q CC\Jmmmr-m~ Aug. 29 -2.0 ter than the A.C. star positions that I·U Sept. 21 -6.4 used. His june 17th path crossed the m Ej> 0^ujU>cr,jcnmu)c» Two of the occultations by (46) Hestia june 17th was AGK3 N10°186 = X02406 " BD uj— c"7cxj·±·F--C that I computed, the ones on June 17 and +09°208, mag. 9.2, spectral type GO, ~ mr~Or—OC^uT = ~ r" 19 (predictions of which were distribut- while the star on june 19th was AGK3 = umnmm~w~ ed in the special notice of June and N10°240 = SAD 92625 = X02491, mag. 8.7, ujuj ¢\JCNCVAJNCVm early July events), were also found by spectral type AO. None of the A.C. = j0cDcomp-7· m ====ujuC> E. Goffin and were published in pages stars that I predict will be occulted "J

'2U' (!j a 2:)" 4'h 40" 20" 0 I , I I I I 0 0 ·,?5" ' 0 0 0 . " .¶43 .0 lElao£jP" 0 ' 0 0 · 0 " P 0 0 " 0 , e ,1 9 , O ® G) · t» 6 V 0 0 0 " 0 9 V . 0 " r, CI) 0 . , 0 ,0

' O 0 0 0 0 _ .. "9 TNJRUS P P ." ,

0 0 "0" K 0 ©:"0 """"""--·-- ...... , , - . +18Cl 0 0gj ---...... 0 :, .O0JT" 0{ , ' m " 0 ·20'- . ,43 " -·-u lj ' ' ' :06

0 0 0 0 o tm0 -Dl...... DC) 0 · , ' / ·-....+ 0 , "":i- :6" 80iCC m. '0 ° · ., . . -··-.-...... " ", 0 · 198/6SEP2! 0 .

0 0 · e / t16 ° Cl) 0 . .\· ': ' '7 ." '. " " K i i i , , b07 , . , · sC 52 50 48 46 44 942· "q¢" "0 + r """"1i . " ·u 0 , . I t986jocr 24 46 hestia M, , · · · 1. " " I I , C, , (I)' , " ° " IDECI2 '50 , ,. . 0 % :(I) AGK3 C)' . · . ° Y"1 jyj 'am'td ' · ,

_. 18 , 4 Ag!),c!) " (I) o (3 'MART5(M-EMAG. (I)'07 ° . ©3O, "0'4 · ',q,,, , 08 °i0f"- d ' 6 0, ' . . 0 0 " " 06 01m " · 0d " 'E"(j)O 0 9 " + - " · · · ° 0µ" " " Go, .· CJ 0 10 0. g

18° 0 — 0 ,C) D 0 · LL +19" 0 %" CI) 0 C" — (I) ®0 " (I) Cl 00 00 (I) 0 " 0 a · — 0' ° 1 0 0 00 E) 0 9) (I) O0 0 M 000 , · , 0 0 ,0 54" / ' 52 3hSO IE '0 "Cl) .$i% 0 +18 - 0 0 0 0 0 ,r- 0 "

1986S£P21 46 HESTIA 0 ,28 '"A CI) 0 7::" CI)" m~ 8 / "7!b 0 8 % 002"7 ,,, ? : ·,0iY" " 'I) 'S%,0 .0 '5 0 0 0 Cl) % 0 % 0 , , : ° b %0 "'% " ,,0 &9 ,0 CC 0 0 O 0 %CI

17°2 Z 0 D _(I) 0 0 8 CI) 00 cp "3 d S ' 0 ," , · " TY .. 0 , (I) I 0 ,p O Qp (i) 0 36" 34 S"32m, +16"'0 m j8I to j 6j4 m 0 0 0 > " 0 0 1986AUG29 46 HESTIA %)0 30 0

16°8 m_ 0C!) ' 0 t!) 0 IS e 0 0 (I) '\8"0 — 0 0 " / O G) Cl TARG T" STA R 0 0 0 0 — ' . i)' ppr am t.vma. Ac. C) 7 Cl CP 00 ° 00 ° ' . ,t h m C "(I) @ 0 ,,,"0/ , '?,b 7,Cb b SO" 48 STAR A3 46 K (I) 80 1 (i · " 2 362 0" If FNKT,oµ A 9 ® /jl2 JO 28 26 24 1986OCT24 46 HESTIA ..V.MA. : C) 917. 6 — q0x3 0 2"2'& 0 , ,9B,6¶0Vl7 46 HESTIA ~~"

0 00 ," 0 MAG. (I) '0 ~8 0 % 0'9« 0 °0 J!) S C) 11 0 0 (S' 15"6 ~0 " . 0 C A 17°2 _ CE) q % H,, 0(9 0"P L 0 12 I m D) M © 15 _ 16 d' . E 29" 27 3h 25" 17 ..(I) · 13 1986AUG23 46 HESTIA IS. 2 — (1)°0% '° ,'0 0

0

// , \\ 14j8 r-m C' ° °: I'L'is - ® 29" 27 g 2 5" ' ' 1986NOV17 46 HESTIA

, ", \," "L} ,7, "j_- )

_ ("' ' \" ,"" -4U' : -.S A" : · :-.""U 'T: m.-. = " ^ " " "' \#" "" ' ' I I " i .m, ' ' i i orl»" " i I I " 0 = m . I I I " C- m· ZK'zm ' —< ' i Ti:, _4 m ,K,,m 4 ,', ' It :),'.~)')) Anonymous by HestiaJ 1986 jul 25 Anonymous by Hestia 1986 Aug 23 4

1986 8 23 (46) FEST 1A DIAP'ETER !33 KM - oho U S * ' - "R j

SeS" ",0, J " " " A %g * ,r "t\ i" $?

3';CJ N . , ,f , G7k "e" · pP t a . / D , 46 - A C" ,K A,p m ' " im" · ' , A ' ." U / · "i 2.6 ' " \ V · p S ! - ./ S 2.a N " . \ , , "" a L2 ,4 R Z / g 35—2,2 TJ N ?5 . LO cr / / St .J ·r uj " O " W 2.CJ N \",i,, ,"wP \$ L * K _ "g / 'a e , * . D —\ ,8 N \" " " © a "

·\ \\ U : 1// , / * ,y 't EREFERIS SOURCE m YECX1ANS '"i" "

- 25—\ .\"6 \ \ CT) / O 0 " I / " m , \ / \ .2 " 7 1 1 L _\ .Cl N\ \ \ V" . / CP. \9. " . O CP \ " B ~ I 1 "a I ,A I "1 \1 :j "" m "" CJ I 5, Cj"O N|o':j N I O.A N\ Cj:2 N I \ " E2 8 & T 'R T

m

LQNGITLEE "R EPFEPERIS SQLRCE - YEQMANS S

W Z ' g'. S

, I ~~ "0 " J7 5H ~ — . " " " D Z CC' j CJ 1986 10 2Q (46) FESTIA — mI 4 DIAPETER ]33 KM - 0 :J q ' Z 70" V q . ·- sG :""" - _ ',!,gH 6 G)i "" · z, pW " ~ ~ Z < , .. 7 \ , , _ , 60 "(9 8 ' ' ,:S S: t\ j S ""' · % " '— Q k-U7 m 'k " — aCT) b——u "' Q " ~ , 9! " * I a LL-I % ~ % 0 L , ,'T OLLJ , ,~ * ©j S gU7 " Z

O IS' i9 ·5 d' CSJ ,9 a "CC' 0 LONG ITUDE ' " " " """'CJ I I I I " d << C" C^ m Q EM-E1°ER[ S SOURCE " YEOMANS G tC' jq f L2 T 5

.

ID OM m P \,: L_

, " . , \\ .\ ,: m = I ~ 'I - J j " ' ~ E D ^N m I "" I ' j " ' . .d "I S , ' .d "I S . . 57 (" . _=3 lV " }-}" qQ % .!,'_.Jl ·' Anonymus by Hestia 1986 Aug 29 .Anonymous by Hestia 1986 Aug 29 Anonymous; bybv HestH&"aa 1986 SCISci) 21

4 n 7 YEOMANSL'42SHIFTnorth

q " J \ >""

, i ' 'mi!µe£'a : \ -r" '\ J" '\j ', ,, , X-= ' m ° , mc/TFe7p= ' ' ' " " " '" " ,. =my'" ' " ' :: Tt " ' '/

Anonymous by Haua'1986 oct 24 Anonymous by Hestia 1986 Nov 17

FROM THE EDITOR inch astrograph, and hoped to provide astrometric updates for several events during the rest of the With the advent of Volume 4, and at the request of year. He listed the events, and asked whether there David Dunham, we initiate a minor change of style; were any other good events that might be included. henceforth, we plan to capitalize Sun, Moon, and I suggested that he might add the events on July 18, Earth, in contrast with our dictionary's admonition, Sept. 29, and Nov. 28. He also said that he was "A capital is used as the initial letter of . . .trying to reorganize the I.A.U. Comiission 20 Work- (17) Names of planets, constellations, asteroids, ing Group on Occultations, and asked if I would stars, and groups of stars, but not sun, earth, and maintain a liaison between the working group and moon unless these are listed with other astronomical IOTA. I agreed to this. names." In the list of events below, those that might be ob- There will be one other change: from now on, we servable with a photoelectric meridian circle (as- plan to number the first page of each issue, as well teroid brighter than 12th mag., elongation greater as the succeeding pages. than 90°) are indicated with an "x" under the "PMC" column, while those listed by Millis that will be attempted with the 18-inch astrograph are noted un- PLANS FOR ASTEROIDAL OCCULTATION UPDATES der the "Lowell" column.

David \A. Dunham 1986 Date Minor Planet PMC Lowell

Mitsuru SOma recently joined the staff of the Tokyo July 18 (6'79) Pax X Astronomical Observatory, where he is working with july 31 (52) Europa x x the photoelectric meridian circle. This instrument Aug. 5 (19) Fortuna x seems to have capabilities similar to the one in Aug. 6 (41) Daphne x x Bordeaux, France, being able to detect objects down Sep. 29 (148) Ga11ia x to about 12th magnitude when they cross the meridian oct. 1 (598) Octavia x (so that their elongation from the Sun must be Oct. 4 (38) Leda x x greater than 90°). He asked me for a list of events oct. 27 (93) Minerva x x which they might be able to observe, which I sent by Nov. 4 (94) Aurora x scanning the asteroid magnitudes and elongations in Nov. 13 (9) Metis x x the list of 1986 events starting on o.n. 3 (14), Nov. 16 110'j(27 EuterpeKlymene x x page 302. Nov. 28 x Dec. 4 (11) Parthenope x Also, Robert Mi11is recently wrote to me, saying Dec. 17 (145) Adeona x that they have improved the guiding for their 18- Dec. 28 (87) Sylvia x x 6

PLANETARY/ASTEROIDAL OCCULTATION PREDICTIONS which is expected if an occultation does occur, Dur is the duration for a central ocCultation computCT David hk Dunham and Jim Stami using the expected diameter of the occulting object, df is a measure of the diffraction effects for a [Ed: This article is a review of the standard in- CCntra1 occultation (it is the time in milliseconds formation needed for interpreting the tables, for between fringes for an airless planet; depending on observing the events, and for reporting the results, the brightness of the star, a visual observer can connected with planetary/asteroida1 occultations. notice a gradual fade or brightening of the star for It consists of extracts from articles by Dunham and 2 or 3 times df, which also can be magnified greatly Stam, which appeared in o.n. 3, with some minor ed- by a nearly grazing geometry), and P is the inverse itorial changes, plus previously unpublished figures of the probability that an occultatTon will occur at for predicted occultations during 1986, including a given place in the possible area, assuming a com- world maps by Mitsuru SOma, and regional maps and bined stellar-ephemeris positional error of i':O finder charts by David Dunham. (that is, t is essentially the ratio of the width of the possibic area of visibility to the expected Predictions of occultations of stars by major and width of the occultation path). The combined posi- minor planets are given in two tables [tables prob- tional error can be reduced considerably with astro- ably will appear in o.n. 4 (2)]. metric observations, and the width of the possible area narrowed to reduce,P. substantially, which can Reports of observations of these events should be be accomplished best wheii the planet and star can be sent to Jim Stann; Rt 13 Box 109; London, KV 40741; photographed on the same plate, perhaps only 2 or 3 " U.S.A.; phone 606,864-7763. Report positive or neg- days before the event. Under Possible Area, the re- ative observations made under good conditions, but gions from which the events may occur with the Sun clouded-out attempts need not be reported. If a below the horizon (unless the star is bright enough definite occultation is seen which could use some to possibly see in daylight) are listed in the analysis for comparison with others, also send cop- chronological order in which the occultation shadow ies to David Dunham; P.0. Box 7488; Silver Spring, will sweep over them. A "?" indicates that an oc- MD 20907; U.S.A., and to the chairman of the Inter- cultation will occur in the area just mentioned only national Astronomical Union's (I.A.U.) Comnission 20 if the actual path shifts n(orth) or s(outh) (the Working Group on Predictions of Occultations by Sat- direction indicated by the letter following the "?") ellites and Minor Planets, who is Robert Millis; Lo- of the nominally predicted path, usually by at least well Observatory; P.0. Box 1269; Flagstaff, AZ a few tenths of an arc second in the sky. The elon- 86002; U.S.A. Alternatively, observers may send gation of the Sun from the planet is given under their reports to their local or regional coordina- El Sun. Under MOON, the elongation from the planet tors, who can then send the results to Stam. Euro- is given under .E),, the percent sunlit ("+" for wax- peans can send their reports to R. Boninsegna; Rue ing and "-" for"Uaning phases) is given under % Sn1, dc Mariembourg, 33; 6381 Dourbes; Belgium. Please and the approximate longitudes from which the Moon indicate on the form to whom copies are being sent. will be above the horizon in the possible area are Preferably, the report forms of the International specified under ljfj. For the latter, the moonrise or Lunar Occultation Centre (ILOC), or the equivalent moonset terminator is specified in degrees of longi- 10TA/ILOC graze report forms, should be used for re- tude E(ast) or W(est) of Greenwich, preceded by a porting timed occultations or appulses. The only letter w(est) or e(ast) to specify the direction in difference from reporting lunar events is that the which the Moon will be above the horizon. "All" or name of the occulting body should be written promin- "none" is used to specify whether the Moon is up, Or ently at the top of the form, and the report should not, respectively, in the entire possible area if it "" not be sent to the ILOC in japan. copies of the re- is not crossed by the moonrise or moonset termina- port form can be obtained from ILOC, from IOTA (ad- tor. The source for the occulting body's ephemeris dress in masthead), from Stam, From Dunham, or from is given in the last column. For most asteroids, Don Stockbauer; 2846 Mayflower Landing; Webster, TX Dunham has generated the ephemeris by numerically 77598; U.S.A. integrating the orbital elements given in the speci- fied source. For the major planets, NA0001 is a U. Sources of Planetary Occultations: [The sources for S. Naval Observatory data set; empirical corrections these predictions vary from time to time, so this have been added in the case of Neptune to make it subject will be covered in individual future arti- agree with the better Jet Propulsion Laboratory's cles, but codes for ephemeris sources are listed in DE96 ephemeris. The orbital elements by the late the next section.] Paul Herget, Cincinnati Observatory, ail have been published in the Minor Planet Circulars (M.P.C.S), Explanation of Data in the First Table: The ranges numbers 4360-4390 (1978 June), 4736-4739 (1979 of Universal Time are the time of central occulta- June), 4824-4825 (1979 August), and 6190-6191 (1981 tion (apparent closest approach to the center of the August). EMP stands for the Lenigrad Ephemerides of object) and are given in increasing order. If the Minor Planets, while ITA-B stands for their Insti- occultation shadow will sweep.across land areas dur- tute of Theoretical Astronomy Bulletin, followed by ing nighttime within four minutes, only one (middle) its number. APAENAXX refers to Astronomical Papers time is given. Under PLANET, mv is the visual mag- prepared for use of the American Ephemeris and Nau- nitude (usually, photoelectric V-mag.), and a is the tical Almanac 20. Some orbital elements were sup- geocentric distance in astronomical units. Under plied b¥ R. Branham, U. S. Naval Observatory, before STAR, mv is the visual magnitude (converted to a he published them in the Astron. j. Orbital ele- photoelectric V-mag. scale using data from the SKY- ments by Schmade1 (Astronomisches Rechen-lnstitut, MAP Catalog described in o.n. 1 (16), 161) and Sp is Heidelberg, German Federal Republic) and Sitarsky the spectral type; the approximate equinox 1950 po- (Poland) have been published in recent M.P.C.S. sition also is given. Under OCCULTATION, Am is the Kristensen (University of Arhus, Denmark) has sup- change in visual magnitude of the coalesced images plied some ephemerides. u. S. Naval Observatory 7

Circular No. 162 has been used as the ephemeris the occulting object in degrees/day. Multiply the source for Pluto. W. Landgraf, Max-Planck-lnstitut listed numbers by 2.5 to obtain the angular rate in fiir Aeronomie, Lindau, German Federal Republic is seconds of arc per minute, which is useful for esti- another provider of ephemerides. International Hal- mating when the asteroid's and the star's images ley Watch (IHH) ephemerides for comets Giacobini- will merge, and how long it will be before they can Zinner and Halley have been provided by [km Yeomans, be separated again. Normally, a separation of two jet Propulsion Laboratory. or more seconds of arc will be needed to resolve the objects clearly. The position angle of the occult- One of the most important columns in the table is ing object's motion is given under.PA.. om, since it specifies the observability of the event. A value much less than 1.0 in general means The star's B.D. or C.D. number is given under the QM, that the event can be reliably observed only photo- NO. column. For declination zones north of -22°, electrically; during the occultation by (3) Juno in the number is a B.D. number, while to the south, it 1979 Dec. 11, a Am of 0.4 was timed visually, but is C.D. The -22° zone can be either, although the photoelectric data showed that the reaction times B.D. number is then usually used. C.D. numbers in were 1 second or more. For any occultations by Ura- the -22° zone are about twice as large as the corre- nus or Neptune, the Nn is for the photoelectric in- sponding B.D. numbers for the same stars, or for frared I-magnitude, to take advantage of the plan- stars with similar right ascensions. The star's et's methane absorption bands in the infrared; the double star code is given under,0,. If separate pre- Nn is much smaller, usually unobservable, at visual dictions are given for the two cOmponents, "A" and "-" wavelengths. For occultations by these planets, on- "B" are used, "A" indicating the brighter component. ly an occultation by possible rings, and not by the Otherwise, the code is the same as that used for lu- planet itself, is possible if the name is followed nar occultation predictions as described in "Notice by "-R." to Observers" dated 30 Septmber 1976 distributed by the U. S. Naval Observatory. [The important thing Explanation of Data in the Second Table: The date, is to note that exceedingly accurate information occulting object's name, and the star's SAD number about double stars can be gleaned from timings of are repeated for identification. The minor planet's asteroidal occultations — more than an order of mag- number, the expected diameter in km, and the appar- nitude better than from lunar grazing occultations, ent angular diameter in arc seconds, are given. Un- due to the slower apparent motion of the occulting der RSOl, "Radius of Sphere of Influence," the dis- body with respect to the star, especially with the tance in km from the object is given where the grav- widely ranging position angles of occultation that itational attraction of the object is equal to that will be seen by observers separated by even a few of the Sun, assuming (pessimistically) that the mean kilometers.] density of the asteroid is twice that of the Sun. Satellites are possible for much greater distances, The source used for the star's position and proper since tidal or differential forces determine satel- motion is given under S, according to the following lite capture; according to the theory of three-body codes: A, AGK3; F, FKU; G, Albany General Catalog motion, these forces are proportional to the cube of (G.C., via SAD; positional data old and usually very the ratio of the distances, not the square. Very poor; G.C. data are used in the SAD for most stars few secondary occultations actually have been seen of 6th and 7th mag.); H, positions of faint stars at distances greater than RSOI. The cube ratio usu- derived by A. Klemola from astrographic plates taken ally gives a distance about 100 times the asteroid's at Lick Observatory, Mt. Hamilton, CA; L, positions diameter, which is usually larger than the Earth's determined from plates taken at Lowell Observatory; _ diameter. After RSOI, the taxonomic TYPE is given P, Perth 70; R, positions determined from plates for asteroids, as specified in the Tucson Revised taken at the Royal Greenwich Observatory; S, SAD; X, Index of Asteroid Data (TRIAD) as published in pages USNO XZ-catalog for stars within 6° 40' of the 783-806 of the book Asteroids (see O.N. 2 (g), 104) ecliptic, the limit for Earth-based lunar occulta- and recently updated by Tedesco. The types are de- tions (with some exceptions; see o.n. 2 (6), 60; termined mainly from observations of albedo (reflec- stars with code x south of declination -3° use SAD tance) and spectral characteristics (color), and are data, but are indicated here for possible double named from meteorites with similar properties. star codes derived from lunar occultations or spec- Hence, specific mineralogies are implied, which may troscopy); Y, Yale (for stars south of decl. -3°, not be completely correct. However, most asteroids Yale data are better than Z.C. or G.C.; Wayne War- of a given type probably do have similar composi- ren, Greenbelt, MD, provided these data); and Z, Zo- tions. The nine types are described below: diacal Catalog (Z.C.; but positional data improved with other catalog data for stars north of declina- C low albedo, carbonaceous tion -4°; the Z.C. is a subset of the brighter stars S moderate albedo, silicate of the XZ, but with some positional information in- D low albedo, dark dependent of the SAD for the southern stars; C, Car- F low albedo, flat spectrum te du Ciel (Astrographic Catalog); K, USNO K-catalog M moderate albedo, metallic (Yale stars with no proper motions available); N, P pseudo-M, low albedo, spectra like M N30; and 3, FK3 or AGK3R. If there are two letters E high albedo, enstatite achondrites under S, the second one is the position and proper R moderate to high albedo, red (iron silicates) motion source for the comparison shift data follow- U unclassifiable in the other categories above ing the AGK3 number. AGK3 positions are often bet- ter than SAD positions, but are generally inferior Composite types, such as "CMEU," only mean that the to XZ and Perth positions. The path shift, in the observations exclude the other types, but in such (occultation path) sense, second catalog minus first cases, "M" really means "M or P," and some asteroids catalog, is given under Shift, which is expressed in currently classified M may be P. The first value seconds of arc, to the nOfUTif positive and to the under MOTION is the geocentric angular velocity of south if negative. For instance, -1.00 would mean 8 that the path would be at the southern edge of the northern and southern limits, with U.T. marked at possible area described in the first table, accord- one-minute intervals and labeled at five-minute or ing to the second star catalog. The value in min- ten-minute intervals along the central path. For utes to be added to the U.T. is given under Time. major planets, the limits are not near the central The last two columns give the star's apparent RA. line, and usually only one limit will be shown. and Dec. computed for the time of geocentric con- Sometimes, no limit will be shown, but only a paral- junction, for direct use with setting circles. lel line, or lines, labeled with the distance in arc seconds from the center of the planet. This is of- Ephemerides: [Dunham often computes the paths of ten the case for Uranus and Neptune, when only oc- asteroidal occultations using ephemerides from two cultations by possible rings are predicted. The two different sources. When a significant difference is parallel dashed lines show the central occuitation found from the nominal prediction given in the first path in case the minor planet passes i:O north or table, the information is shown in a third table.] south (measured perpendicularly to its path in the The value in the Shift column gives the path differ- sky) of its predicted path with respect to the star. ences in arc secohdS%easured perpendicular to the Combined ephemeris and star position errors can asteroid's geocentric motion; the letter following cause path shifts this large or larger. Other par- it tells which direction the occultation path will allel lines are sometimes drawn and labeled by hand be displaced on the Earth's surface from the nominal to indicate alternative predictions based on ephem- prediction given in the first table. The value in erides or star positions other than the ones Dunham the A.t. column tells whether the geocentric time of used. The sunrise and/or sunset terminator is closCSt a¶proach will be early (negative) or late shown, with hatches indicating the side of nighttime (positive in minutes relative to the nominal pre- visibility. The star and occulting object are in diction. The EPHEMeris SOURCE is given in the last the zenith for an observer at a site indicated by column; the shifts are in the same sense of the the center of the circular projection of the Earth; source specified in this column minus the nominal the objects are on the horizon for sites at the edge source listed in the first table. Many of the dif- of the circle. The altitude above the horizon can ferences are quite small so that comparison with ev- be estimated for any site shown on the map; the co- en relatively recent observations in the M.P.C.S sine of the altitude is the distance of the site yield only insignificant differences in the residu- from the center of the circle divided by the radius als. In these cases, Dunham's predictions usually of the circle. The Sun altitude can be estimated agree well with those by Wasserman et al., except from the terminator. sometimes when different stellar data are used; they usually use AGK3 data, whereas Dunham uses data from Regional Maps: The more detailed regional maps are other catalogs, when available. prepared with a computer program originally written by Fred Espenak at Goddard Space Flight Center, and Maps and Finder Charts: A map showing Dunham's pre- extensively modified by Dunham. The parallel curves dicted paths of asteroidal occultations during the represent the path of the center of the occultation year in the U.S.A., southern Canada, and northern shadow, considering several different shifts of the Mexico is routinely published in the january issue occulting object from its predicted path with re- of Sky and Telescope. Dunham's finder charts are spect to the star. The nominal path is labeled "0" published in o.n. for individual events potentially and is drawn slightly heavier than the other paths. visible from North America and Europe. Others usu- The parallel curves show the central path for multi- ally are distributed to observers or to regional co- ples of 0'!1 shifts of the asteroid from its predict- ordinators who further distribute the charts. [The ed path in the sky, measured perpendicularly to the charts may or may not contain a small-scale section path. Curves are labeled in the map margins with """ taken from a published star atlas, depending on "N" or "S" showing shift direction; "E" or "W" are whether or not there are familiar stars or star used if the occulting object's motion is nearly due groupings in an accompanying computer-produced 3°- north-south. Dashed curves show predicted U.T. of square enlarged chart; the 3°-square chart may con- central occultation, or of closest approach. Low stitute the only chart, or there may be a further star altitude or twilight boundaries are drawn when enlargement to a 1°-square chart; or the 1°-square appropriate. A stippled line marks the moonrise or chart may stand alone.] On at least the largest- moonset line, if either is present. The expected scale chart, the path of the path of the asteroid is diameter of the occulting object, in km and in arc shown, with Oh U.T. tick marks for four dates start- seconds, is given in the heading. The ephemeris ing with the date two days before the date of the source is indicated below the map; the stellar data event. Hence, there will be three tick marks on the used are indicated by the first entry under the "S" side of the occulted star before the event, and one column of the second table. Dashed curves parallel mark after. Close double stars are underlined. For to the solid curves indicate predictions for the stars fainter than 8th magnitude, Dunham has com- path center based on other stellar and/or ephemeris pared the detailed charts with Papadopoulos' True data, as labeled. Asterisks show the locations of Visual Magnitude Atlas tO add some 11th and even observatories from which photoelectric occultation 12th mag. stars in the vicinity of the star to be observations have been attwpted in the past, as far occulted. This comparison also serves as a final as Dunham knows. The regional maps are "false" pro- check of the chart against a very close equivalent jections, plotted with a constant linear scale (con- of the visual appearance of the actual sky. stant degrees per centimeter) in both longitude and latitude, sq that the reader could, for example, World Maps: Mitsuru SOma, Tokyo, Japan, produces plot updated computed path points which might be the world maps published in o.n. by computer, using provided by Lowell Observatory. An updated predic- stellar and ephemeris input data supplied by Dunham tion by Dunham usually is given as a ?ath shift in in machine-readable form. For asteroids and satel- arc seconds, which can be interpolated between the lites, the three closely spaced parallel lines show adjacent solid curves on the regional map, and a cor- the predicted central occultation line, and the rection to the time, either earlier or later than the 9

time estimated for a given location from the map by fore the time of closest approach; this will give interpolating between the dashed U.T. curves. If confidence that the correct star has been identi- the correction to the time is very large, the con- fied. With a larger aperture, there will be a high- tinents will be shifted in longitude relative to the er signal-to-noise ratio, so that an occultation occultation curves due to the rotation of the Earth, will be more clearly visible. If the asteroid is and the path shifts consequently will be slightly not visible, and the star appears faint, dimnings different along curved paths. This effect is great- due to atmospheric seeing variations are likely to est for paths extending nearly due north-south, and be mistaken for occultation events. Since separa- is inconsequential for east-west paths. Dunham tions of only a few thousandths of an arc second of- takes this effect into account when he derives an ten can be resolved during an asteroidal occulta- updated path shift value, using an average value for tion, very close double stars sometimes are discov- a given regional map since the error in doing this ered. The ability to see imersions and emersions is almost always less than the uncertainty of the ' occur in steps due to duplicity is better if the astrometric update. Regional maps usually will be star appears brighter. published in o.n. only for occultations potentially visible from Europe Or North America. Regional maps The value of practice in locating the target star for other areas with at least a few IOTA members are before the night of the occultation can not be over- distributed to coordinators for further distribution. emphasized. A good finder scope, able to see stars to about 8th mag. and with at least a 5° field of Dunham finds that his paths often differ from Gof- view, is highly recomended. On your first try, al- '"" fin's by a few to several tenths of an arc second, low at least 30 minutes to find a star in a diffi- so that producing SOma's world maps for all listed cult field, such as one more than 2" from a 3rd-mag. events does not always duplicate Goffin's maps, and star, especially if strong moonlight is present. also gives the better events worldwide, rather than After a little practice, you will be able to locate just regional, distribution. He is now producing the target star quickly, an ability which may be im- fewer finder charts, because Goffin's charts usually portant during the night of the event, especially are adequate. His finder charts are mainly for for those traveling relatively great distances with faint stars (where the A.C. plots are helpful), for portable equiµnent. If :your telescope is equatori- some events (mainly due to star catalogs not used by ally mounted and has setting circles, practice using Goffin) found by Lowell but not by Goffin, and for them to offset from a nearby bright star to the tar- some bright stars where not enough faint stars to be get star. seen in a telescopic field are included in Goffin's The best current method of recording an occultation charts. is with a high-speed photoelectric photometer. Al- Local Circumstances: Predictions of local circum- though this has been almost exclusively the domain stances of planetary occultations and appuises, of professional astronomers at major observatories, which supplement the tables of general data given in designs and components for relatively inexpensive o.n., are computed and distributed to all IOTA mem- photometric systems have been, or are being, assem- bers by joseph E. Carroll; 4261 Queen's Way; Minne- bled at the University of Texas and at Lowell Obser- tonka, MN 55345; U.S.A., telephone 612,938-4028. vatory. News of these systeirs will be announced in These predictions are available to non-IOTA members o.n. as they become aVailable; eventually, it is by sending Mr. Carroll accurate geographical coordi- hoped that at least one of the systems will be mar- nates and $1.00, payable to IOTA; processing of re- keted connercially in completely assembled (or near- quests will be speeded up by supplying a S.A.S.E. ly SO) form. Other automatic recording methods in- clude video and photography. Paul Maley has photo- Since the computer program producing these predic- graphed breaks in star trails during occultations of tions was originally written by Dunham, and since he relatively bright stars with an unguided 9-cm aper- provides the input data used by Carroll, Dunham's ture telescope. and Carroll's calculations are mutually consistent. For each input event, the local circumstances print- The best way to record a visual observation is to ed include the U.T. and distance (in arc seconds, tape record event marks and coments along with kilometers, and diameters of the occulting object) short-wave radio time signals. This is better than of closest approach, and the altitude and azimuth of using a stopwatch since the record can be replayed the occulted star, the Sun, and the Moon. No data several times, to refine the time of marked events; are printed if the star is below the horizon more multiple events in quick succession can be recorded; than an amount proportional to an estimate of the and rmrks about observing conditions and interrup- occulting object's along-track (time) error, or if tions can be included in the timed record. Events the star is fainter than 6th mag. in daylight. can be marked either by voice or (perhaps prefera- bly, since hand reactions may be quicker than voice) Observational Methods: Numerous techniques and by a mechanical clicker or electronic tone genera- hints for observing planetary occultations have been tor, such as a doorbell. Valuable practice can be discussed in previous articles on predicted and ob- gained by timing some lunar occultations; see Dun- served events in o.n. and in Sky and Telescope, es- ham's "Occultation Highlights" articles in each jan- pecially in Dunham's annual article in the january uary's issue of Sky and Telescope if you currently issue of the latter. Some of the more important do not have predictions for your location. Field methods and considerations are described below. experience gained from timing multiple events during a lunar grazing occultation can be especially useful Use the telescope with the largest aperture availa- for observing asteroidal occultations with portable ble, to give the brightest-possible image of the equipment target star. Also, with a larger aperture, you are more likely to see the asteroid approaching the Single observations of asteroidal occultations pro- star, 30 to 10 minutes (depending on the motion) be- vide a very accurate astrometric measurement of the ]0

asteroid relative to the star, but tell us little night during the appuise, but the possibility of about the occulting object. Asteroidal occultations such an event occurring, though always low, increas- are best observed as a group or regional project. An es considerably as one approaches the actual occul- example of such is Stann's Asteroid Research Pro- tatioh path. Secondary occultations almost never ject (A.R.P.), which was organized for the pupose of have been reported more than ten diameters away from confirming asteroid duplicity, by having as many ob- the asteroid. This fact also can be used to plan servers as possible monitor asteroid appulses as the period of observation and recording (be sure you well as occultations, within the contiguous 48 have enough tape). Start observing at least ten states; additional participants are sought (see o.n. times the predicted central duration before the pre- 3 (7), 148); contact Stam. At least two, and pref- dicted time of closest approach (and add to this the erably three or more, well-distributed chords uncertainty of the time of closest approach), and (ideally, one near the center and one near each of continue for at least as long a period afterward. the limits) are needed in order to determine the as- Stamn previously suggested observing for the number teroid's mean diameter reliably. Consequently, when of minutes equal to the number of seconds of maximum last-minute astrometry shows that an occultation duration, with a minimum of 10 minutes, and a maxi- might be visible from your region, as many observers mum of 40 minutes, but now feels that the minimum as possible in cities and towns throughout the re- observing time should be extended to 15 or 20 min- " gion should be notified. Gall's Astronomical Direc- utes (see o.n. 3 (IS), 327). But be careful not to tory and the Tnternational Directory of Amateur As- become too fatigued; try to arrange a comfortable tronomical Societies are both arranged geographical- observing position, and take a brief break (note ly and, along with some directories of national pro- when you do this) if you start to become too tired. fessional societies, are useful for contacting po- Be sure to be especially alert during the three or tential observers. For events visible from North four minutes bracketing the time of closest approach. America, finder charts often are published in Sky and Telescope, tO which most non-o.N. subscribers Prediction Updates: The predictions for asteroidal can be referred. But most important, observers with occultations can be improved by astrometric observa- portable equipment are needed to travel to locations tions to update the ephemeris and the star's posi- between cities with observers, to fill gaps in cov- tion a few months in advance. The improvement can erage and increase the chances of obtaining enough be quite good if the asteroid happens to pass near well-distributed chords. The deployment is a little the star, perhaps during its retrograde loop, so like that for a lunar grazing occultation, but on a that both objects can be photographed on the same much larger scale. The observing "fence" is much plate. Sometimes these preliminary prediction im- longer, to cover both the asteroid's diameter and provements are published in o.n. or in Sky and Tele- the prediction uncertainty; observers generally are scope, or distributed by Lowell Observatory astrono- separated by tens of kilometers. When possible, mers or by Dunham. However, a very accurate predic- visual observers should observe in pairs, separated tion generally can not be made until the objects are by a km or more to confirm each other's timings by close enough together to photograph on the same as- independent observation not affected by the same lo- trographic plate during their final approach, only a cal atmospheric seeing cell or cloud. If the motion few days before the event. In these cases, those of the occultation shadow is relatively slow, the involved with computing the final predictions must observers of a pair might separate themselves along concentrate on notifying those near the path; this "" the direction of motion by a distance large enough is facilitated if those contacted will telephone to produce a time difference of 2 seconds or more; other observers in their areas. the regional map can be measured to tell how large a distance this would be. This will not only allow You can find out the latest predicted shift and time confirmation of observed occultations, but also will correction for upcoming asteroidal 0ccu)tations by permit a rough measurement of the motion of the oc- telephoning one of the following: culting object. This would be valuable for estab- Hans-j. Bode, Hannover, G.F.R. City code 511,424288 lishing that a secondary occultation was caused by a body which shared the motion of the asteroid. Coor- Astr. Soc. of Harrisburg Obs. (PA) 717,938-6041 dinators need to balance the need for a large-enough David Dunham, Silver Spring, MD 301,585-0989 number of observers across the zone of prediction uncertainty to obtain enough well-distributed chords Astro-Alert, Chicago, IL 312,259-2376 across the asteroid, with the need for confirmed ob- Paul Ma1ey, Houston, TX 713,488-6871 servations by pairs of observers; the available man- power is always limited. Observers in cities rela- Lowell Observatory, Flagstaff, AZ 602,774-3358 tively far from the predicted path, who can not Also in Silver Spring, Joan Dunham's ASTBBS probably travel to it, should observe also, in case of astro- will make updates available to anyone with a termin- metric error or to observe a possible secondary dc- al (or personal computer) and modem 301,495-9062 cuitation. But in such cases, visual observers al- ways should make an effort to observe in separated For some very important events in North America, ar- pairs, as noted above, for confirmation. A second- rangements will be made to broadcast prediction up- ary occultation by an asteroidal satellite is possi- dates on HWY at hourly intervals during the few days ble for anyone who has the star above his horizon at before the occultation. '"r " n^kN~]"

%} " !' '"",=/'/'' ::''' tj" "" ':< ,, '\'\"

} " ,/ :¢:,')'j\ ., j , 7>'t":}"~, ,rt1-¶ 'j L ' " " . ' '<' 4 a/j· ·U U <¶,J >, ~ b , , ,0 ·n ~ r I-A I 4 I -U I, U I,, r ' " 1^, :ddk 6 , n ID,, i t 'm I m \ ,, i : \ , I 7 . S1\ \ ': K—m to ·. / S u

G ' ,, ,, J t,L , ,A, ^. Cj\ , ""

SAD 163645 by Russia 1986 Aug 10 SAD 138759 by Venus 1986 Aug 14 SAD 138883 by Venus 1986 Aug 18 ~ r" _ + , 7"

—- h 5" I ~. I m'6 ' I I'I, " '1\J I 7 j _ m Q Q , 7 I m I "

L. ·44 "u - 00 " 0 - b. I I " U j I I @ 0 " " > (,\\ _ "'.'. 10 u ' '

k ~ + SAD 185266 by Lilea 1986 Aug 21 SAD 139183 by Venus 1986 Aug 26 SAD 94719 by Papagena 1986 Aug 28

M ' I ;'

g \"

, \\'

I I

I '\,\ I " a , . . , P

h

_ , ,,1/ ~_

— =2!25: ;±c '± Klutcs.r% E's,f" m q" SAD 111430 by Adeona 1986 Aug 29 SAD 187784 by Mars 1986 Sep 6 SAD 211769 by Sabauda 1986 Sep 7

r (_ L m " % :, D ":Z7 '_1J —¶. s"??I " < " ' ( , _. G ' 'J 75 Q L'sh SID ' » _ j G lj U V < i 0 N. . 7 ' ~ ~ h m E N m 'r

W . D ~ . I b L

SAD 182536 by Bertha 1986 Sep 7SAD 158288 by Venus 1986 Sep 11 DM +33°1391 by Alauda 1986 Sep 18 12

" + 35 " PEGASUS '4° D O C) 03 ° CI) 0 e 3C . J: " " 0

06 · VI ' e 0 0 " D , 0 3 0 , jCt) O Q "¢0 5j , , Hscej . 0" " " )0 q_ -(I) 0 "

" , a ,j _ , , ,, 0 ° ' 0 o " "·7... - ·5" m"~ ' ° (j 2· 8 " Q 0 0 CJN 0 e - "".. 0 ~ % O O

% . , .. % 0 , 0 0 CJ 0 """""- ' " ' 0 I? ,2 -9 CJ CI CI) O ,— 0 C) C J " · ''" :S'-- ... , 22" Cl) O CI C: 0 0 0 0 0

¶P " . """- " · ' '21 0' 2 ,"4 _ 0 :'yy ;""-:,, 25 , Cl 0 q°

· """ m 0 I 'J I13I Cl 0 ® " 0 1 I , (E'uf i · ' " . -.. . m '?!k m ! 0 e ., ' '-..,"·... . - 0" !0 8 6 4 2 0h(r 6m m ° 0 . " ID' · ·-.. 1986OCT 27 9J 4INERVA 4 D 2 /4 , ""--.. "0 1986OCT27 93 MINERVA 0 . b

D , : , 0 """-.. . BD +02 4754 0 0 0 : 0 g · , 0 " · % 20 , ' " . j4 , ". i . "" .% # 0 '27 jll " . · . cjm&83 REGulu^"

P · Hz i , D Aquarius 0 "" ·18° "5 @J 0 - 0 0 ·- 3'0

C!) S S ° O 0'g "' '"" 0

0 " 9 bQj0 ° 0 © O" '9 °d 0 ' 0° " " ' ..-"°""0r·.-K""" " . D (I) 00 +4 -· 0" 0)( ... ·"'"""""°" 0 . "'7 " Cl) 0 D 0 0' b, , °0 0 0 .. ...·""" 4¶V; . '1¶ ' cS\"K ° 00 (9 ' ''" ' ° ·-""""";e;"""""":tc i;a;"33 "'°. .¶3 ,

'3 0 '" .· . 0 . : Sc X LANI ' · 0 0 . +16 - 0 +3 -CI) " q " 0 |? ac3 " 0 ° 0 · ' 00 CI) · "" 0 . 0 G) i . ° %' oy " (g , D " '»58 ,:· · + .·" au· 8 0 % 0 ° ' , ° " " ,,,· , , HYA,PES , , , 0 , , I ° In ('I " 36 ' ° " ;3 " 26" 24 n 20 IB 16 C,r "2 ,2 40 J8 36 J4 J2 10jQ : .

7986DEC22 877 WLKURE SAD 93900 1986NDV19 IS EUNOUJA BD +0j 2400 + "' · " 0 g 26 "0 """ " ° ° "" ' % " :3 O U 0 0 3 C' :° ° · , 0 0& "C) , 0 e O _ % ©°°30" 08 0 0° 0 +1 4 2 " 0 O 0 JO 0 0 0 ',

" 13. 2 ± ". L0 0 0 0 ° " 0 j O 0 O (3 25 6 "0 DJ , ,joj 0 O 0 3 '% · 0 , 3 «T 7!0P It . © :(1) °3, ."q ' 0 0 0 ~~L 0 0 g +1j _ , O 0 "0 ' 0 0 0 '3 . (I) (3 .

0 . n " 0 " 25"2 _:° , 0 : '08(!)" 0 0 · 3)2?8 :T- 0 g 0 0 +it I ° I I A (I) I 0 42" 40 JB J6 J4 32 SJ0" 38" 36 g 3T CB i 2 5 m 2 3 !986DEC 12 377 CAUPANIA SAD 9JSJ4 2h 2 r 1986DEC12 377CAHPANIA SAD 93534 1986OCT 4 38 LEDA SAD 75363

B 0 U 30" 0 — 0 ? % ° 20? d —0 00 0 :e 3 U (!4b 0 D O D cP O , 0 0 . (i 0 0 0 " 12°4 —CI 00 0 0 W 0 O 0 00 G 0 a 2°: 0 qO QJ3 O O 0 m 0 0 0 , 0D0 O 0 29 6 :Ch " QC) ° 3 O 0 O 'S It @,0 % 20 d 7¶ ,YN " 0 'p. , CB , t9 G) 0 , (3 3 eh!) HOV 0 1 2. 0 —" Q) T, , 0" ' '1 ° ,9 ,3'3 0 NoV 11 'Z 0· 0 CD 0 0 3 Q T": 0% 3 · 0 0 0 3 " Q)" 0 0,CJ e 3 0 0 0 0 0 0 X 'r' :j, , , !°": µ, % : , 20:0T , (b " 0 9 11"6 a— 0 0 i ' I m 9" 7 8h 5" J3" C) 31 4h2sr 28" 26 24 24" 1986NOV 4 94 AURORA SAD 79994 1986Ngv13 9 UETIS 1986NOV16 27 EUTERPE _1 gO O 0 0 0 Q " Q 2SFZ J '3 (8 , (JJ O 0 D C3 3 _ praesepe ui ,(J ; ° 0 ,¢gb gO _ D 0 0 8 3 " ,9 Q 0 (3 '°"'siz¢,°';i°: -20 - , 0

0 , ,0000 ci)' , " :.. " Ej'< " · u d " -$0 0 rP0 KJ Q 00 . )5 0 " jt " · Nov AT g o u _ %Q. ,°· ' ° '0 (I) 6 ·0 ? , 0 00 0 7 "2' - ,, "c!)g 0 , , 0"0 0 0 . 0 D ,,oC)" " " .: : , 0 24"4 — 0 M (i " '°°' 9j% ', & 3j ° g,:c, : : ZL & ° ·· opHiU(jWf O 0 3 °(je$ 0 O 0 90 0 ¶(LMN1 Op RQ Doc) -22" I " , , , 0· % 22" 20 IB 16 ) 4)2 1 7\ 0" 55" 5J 4b' S r 38" 36 jjh n

\986AUG21 2¶JL]LAEA SAD 185266 19136NOV28 104KLYVENE SAD 70849 1986D£C30 946POES!A SAijdjj22 13

]986 B 2J (2!3) LILAEA SAD 185266 1986 9 29 (148) GALLIA SAD 167259 DI AI'ETER 105 KM = 1j:OB DIAPETER 92 KM = OXJ9 EAJ" 55"

, ., " D Q 8 Q Z D . ,f d 55 ",,J / , M b G ' 1 / :,? ,, (? * 4,p / " _ ' ' ub £ / / W 45 , " F ,// T ,, jM Q / / 4 * ' L .t / // / W " " ' " " A ' , / '/"',,"F7/" · -t-''·" : 45 9,/ / 1/ " L * W

[ :.,,, / . j§ · !,,3 :- , /1/' '/Z Z Z<;

W E Q't / / ' U ,> , " ",W L':g 3. E ,— 'T * IF C" ' ~ B 35 "Q/? S r%/"~ ', " ' / '0L ' ? 0~ Z / / ' "+ >' '9· "V " / K 7 " ;;"' , /$ y ' ^ / 25 C J " 6 ¥ ,SQiS°j , " ,, 'E"" / 1 t/? '? ' 0 ,1 * G 4 ',:;; ,? ',.: ;; : O :; O9 "":' ." : "CCb, " -20" -10 0 to 20 30"

LONGITUDE , .< X > iS I " j-S 1 O I I '' I'D EM-EMERIS SOURCE - Erp ]98] -130" -120 -no -jot) -90 -BD"

LONGITUDE

EF¶-EPER15 SOLRCE - EPP ]98]

1986 JO 4(38) LEDA SAD 75363 DIAPETER 1]8 KM - oho 55° ' :'C '" 2. n N j°? N I ," )))"/"".,.'))'),, )

! "!:' ' "%( '='SJ" :' " 'T" ' "t ' E

D 0.2 S '!21 ' ,, N, ., / , ~ / " E 1 K "' V IN * * u m. 4 S 1 , / i

0 0.6 S I , ' I V. m 1 . I / S " 25 -0.8 S I I " '\ , O I I I I / 1.0 S I ~~~_ 1 I 0 d t·2 S I I P V " ,, I I / I .'4 S I R C> 'E, iS I I I I 1 I -130' -120 -I JO moo -90 -80 -70'

LONGI TUDE

EPFEIERIS SOURCE " Ell' 1986 14

~ ~gh 15m 00 ~ !"jz\" IB ,/ —-mo - I f ' .J " J J m= · T""T S " b—u 0 q dj 6 Q |0 I I j ~, bO 0 0 I bO 0 I h m i -.'. .,.. 19 0 . ql cC , I , I f> 0 D " I t

t

I

3

q P ~

SAD 182838 by Venus 1986 Sep 28 SAD 167259 by Ga11ia 1986 Sep 29 LJ 1691 by Parthenope 1986 Sep 29 \ mmm"~¶ / II i ' '.

0

0 0 7 SC m i I 14 ' "'_~L Q " ,,F"r 0" I I " IQ " 3 I 0 I |0" I to b I 0 00 A Q I ~ ID ID u I 00 4 Q ' "tt U ,, 0 I C 00

~

" . JO

SAD 166016 by Octavia 1986 Oct 1 SAD 182934 by Venus 1986 Oct 1 SAD '75363 by Leda 1986 Oct 4

" pm m \ ~. " ij" " ; '"I f \ _

k 7 1 I Ik , \ ~1) ' ' S" _ "/,' /'/ "j ;X,-i e · ' \ '° t h 'T—ji i ,, . -m ,, , qP /E,,:7- -,'/ ,,1 1 "\ , I 4 \ e 3

O \

C7 '"UJ)jj O \ 0 Q 'C7 r ~ X, 'Q 'O ' Q SAD 189038 by Mars 1986 Oct 9 DM '02°4754 by Minerva 1986 Oct 27 SAD 98854 by Lutetia 1986 Oct 29

DR

11 2 ~ a 0 ( A 0 I 0 L 3 0 ' 0 Q ° . I ' , 0 V I 11' , /

« I _ I p % = j m ,0 " Q CI Cl

SAD 79994 by Aurora 1986 Nov 4 SAD 190724 by Isis 1986 Nov 6 SAD 190516 by Dembowska '86 Nov IQ 15

1986 JO 27 (93) M 1NERVA BD '02" 4754 DIAPETER 173 KM - oM

70° 4 C

\ \ 65 : X \ \

,, , m,,,,7 2" ", l"'\ bi,8° J6—"', I W " ""' ,, U ' , \ _:

, , , A .6 N \ · \. \ , I T \ ' 'CJ;f \ " \" ·1 |a Cl t j.4 N \ \83 : "- ' \ \ t

E :j.2 N \ P " \ I " \ "D \(P5 \")" \ 4 I

35 ±2 S \y5 · '\ ·\ S ' \ <1 I —" " :J. 4 S \ _—" dj J " ~ 0 \ I ,6 S \ _ , ~""L " \ :! L " ' , ' I

,,; I 'I I I S I ,: S .1 I -20" -JO 0 10 20 30 40 SO"

LONGITUjE

EppErERls source - epp j9bj

1986 I] 4(94) AURORA SAD 79994 D IAPETER 191 KM - 0."10

0 55 ,,5 a 0_. "G '

' X % j \ j " j \ j _ _ * \ i J —Ip' r ~ _ " r' \i f " " \ .0 J . " , " " ' , ,27^ r' * ,, ,,, , > ,2" , ,, , , . , _ \ " m " ' 1^/ I " N "" 1 , ' P" . ,. ,, , S \ \ cP+ — " " I,,7 , . K " S " _ !, ":S°" .. . ,><1 " I < · ': ' ) O ccF ' " O i+ " · ", ", ^Y ,' " . \ .I \ \ \ \ O J " I a I \ 25 —J I/ / , '\ XJ ), * . \ \' \ \ \ 2 3 T' \ 0 \

jr " v " ,g °;'+jO C,'"O."L:, Q5 "%O>:jS' , 50: p ,,>>sj,. 1+ ,Jy

-]30' -120 -no moo -90 -BD -70 -60 -SCI'

LONGI TUDE

EPFEPERIS SOURCE m EFP 19Elj 16

h m

T .

I I ''" '7 '

Ii Ll Iir-r_"j"i 5 t Qq Ii,'C' tt

D aQ PO Cl L5 m |5'E/5 ·1 } L5 m |5'E/5Jn j' 45" q Q 0 L m6· 0- 0 / " 6 L m6' 0i -

ID '

45m

DM "20°775 by Metis 1986 Nov 13 DM +18°721 by Prymno 1986 Nov 14 N10 154 by Havnia 1986 Nov 15

, -K"=f~. I . 63O ' ' "' 4 /7/ "~ \\ ,

0 { ---- 3 cr 0 S 35m 4 ~ ~ m \, 3~ J "L_ " (i ' ' '"' " 'tr j ," h r ° ° ° 1 0 0 ^ 1\'\ t I · 0 - }- "L'\,\"\,\J,,\ .I ,',tit/j I

" "".mx: " "" I ,J r DM +11°344 by Euterpe 1986 Nov 16 DM "03°2400 by Eunomia 1986 Nov 19 SAD 76849 by Klymene 1986 Nov 28

]9'?5" i I

q #1¥im / 'I! 7 ',:\,

Z'- , . 1 G

. .S LO , 0 ,J :=f := I 0 I/ ' j I I I II 0 0 h 25" \ \t 10 " 4 '<1 " \\ ,: .:m iih'°00 . \,\,\ ': , /, Cg!£} _ _ _

SAD 165064 by Mars 1986 Dec 1 SAD 96444 by Parthenope 1986 Dec 4SAD 93534 by Campania 1986 Dec 12

.~ .0

/1. "lV

I . . ., ID

. 0 22 b i JO i I

I b " I n " m -g 'g ,'" 5, '"° Bh 0" 77L5L55"_ h AG j t r I _ t" I/E \ , 7 h , 0 _ I I I , \ ° X) . 0 I,? N

Jl a0 L \ :0 " ·0 \ I;? »0 \ 00bn .0 " 31j?q \ \ ' ~~ I "; SAD 158670 by Venus 1986 Dec 13 SAD 93262 by Adeona 1986 Dec 17 SAD 93900 by \4a1kure 1986 Dec 22 17

1986 11 13 (9) PETIS % "2cf 775 '5 DIAIETER 19U m - 0:2'3 704 U:'6- S a ¶ S '·? K _ — Q;' C ^":?

P si'"!- — " " 'j,b "3I-q""S ' " - "" "" jb"O — ( D) I" , 1· ,2 S I _ , ' V i g, 60 — '. 1 S' / ' DQ & ,1 " " j b ~ " · ' Q i \3 « - CJ'7 ,0/ " i L . 0 IQ i * A " / r· V' * t * T S — ~ & ~ : SO — 2' S' ' :" ' ^"" k+ m " ' 8 CV R * U 2- ' % I 8 b D 2·6 S . 7\:. _' f E 3-jj S u / E . , ·,1 tn \_-- , ' S0 7 & q ' S , It! " I ' " · ·" "" ':: 40 · ' SQ " % m CL :k a. 0 , 0 , 'T " Ei / " , d_ * _ U7 * * U1

u cn E" — CJ

wm uj 8 qr f 30¶ I I I I 1\ m ,,/ " "F " "' - ? -1(J° 0 to 20 30 4J 50' ~ / CJ / LONGITLAjE EFFEJ1ERIS SOURCE - BRANHA11 * * , " " 3" ,1 T I * " " °mr °. R 0 t 4, % ,S, 'P, % %%'si":%%y* _ T 's'g. \S' 1986 jl ]9 (IS) EUNOMIA BD '03" 2QOlj \"" C" ". ae, ii - '0 b DIAPETER 26] KM = oM 70" /'""6' N I d' N / c9 4, ?9 V '3 i t ? ¥ '"'is: "" ' k7 1·5 N // ( .j<+—r-»cjuj

65 -L. ¶ / /

jd 'V ¶ I 1/ , l|'? 'V g / Q & Q

' 4, / / , . 55" |O N

j S9 N 1/ * . T -) '19 4, , , N e 1986 11 19 (!fj) EUNM!A BD ·{)3"2400 : '7 N / , / DIAJ'ETER 261 m " 0."13 : " Q'), , ':' S, 55" Ui ft , ' ::: b, : ! t (J. \,J\

, gO" \'t,J\ L " 3 0 I A ' 0.2 ,5 ;!:,' "° T 1 45 "' -0_ : Sad , '2 "St",o,j=y="^30. 2 S : W;:"S,X / 6-· 0. 3 S ~b3

S O:q S > 2qj \1 I I I I 3!1' ,I I' " -aj' -10 0 to 20 30" -75 -65 -55 -SO"

LONGITUDE LONG 1TUDE

EM PER15 SOLRCE - ERAMIAP1 EPFEIER IS SOURCE - BRAMAH 18

!986 i! 16 (27) EUTERPE BD 'I r 344 D [METER !16 KM " 0."!5

55" d

V

, \ \ \ " \ \ \ ""= 3. A ' ' I 3 ,:i N " \ ' \ i \, 45 3 Cl " \ , ,1 ,0 N I \ 4 * "K _ , \ .t 6 N \ N \ ,or " W " \

A N + " 0 ) ,, ;:: , '1 , " ' K^" · · · °

J N " : "S k 3 3 ' )'1:" ,' "' " ' 25 (j.O N " °':: \ . - ',

.Z N \ ' \ , \ \ \ \ \ " . , fj.Z A S D. jj.8 \.g 5 \ .2 \." \ 5 2. 5|2." S .6 5, I I 15 , -130° -!20 -I !0 moo -90 -80 -70 -60 -SO

LONGITUDE

EPHEPERIS SOURCE m HERGET77

1986 I! 2E) (104) KI-WERE SAD 76849 1986 J2 IMARS SAD 1650EN ~~- DIAFETER 13Q KM - [j:|l diafeter 6782 Krj - e3?'3 "' "'j':", ', :"' "" "is '" "" Qi '°" ' ~

SO . "" 65 - Ee 6 ° 'I ~ Z"' g Q, " Cj _ °':;"OO:S " " "% " C 'J,; " )'° -i't" " ,' ':· I ' t , ] 5( ,Q 81k G 'b· I, )T 55 , C,. cgo I T ^':n / U _ O> a U _ k 'J · « D a ,? S" ' D k' " ' 30 :°2' ", :, i ^,, ,,'· t. E ,gc' * * 45 -S' "

, D

Q ' " 0 d: % e8 Cj% ' ,'

20" I I I I I I r 34 n) ' G" I 'I I rj, ' I ml -·130' -120 -I JO moo -90" -10" 0 to 20 30 qo"

LONG ITUDE LONGI TIRE

EPHEPER15 SOURCE " EPP 1983 EPHEMERIS SOURCE " NA0001 H

.b

' % 19

d L "n'f' :S t! E > 0', td

i, !:)1" "'[ :"'"^'"' '"""i' , 1986 J2 26 (238) HYPATIA SAD 155?042 D) b )1 a DIAMETER 155 KM - OUj6 t E " _m_ '- - -&gE55". ?' g Ai ' N 2"-j 1\, 1

K \ «J Cp

%b j

!:r· LLJ "\'-dr * · iiin m D— · * <" 0 "' 'b ^ ' -- jz \ ,_ __ ,, _ _ - ;? i \ k \ \ 45 2.jj r , \ \C',j". ,- \ \ , \ gr " 'C$^" "9 lV \ , 'S ',\ , ~\ * \" · L ' " " " a " CJ ,A ' 'N , \ · ,*\\jj_, m ' 4t<""0 J e7 " ·· ~ 7" f TI * ~ 35 I' 7 M , \ H \ gf ? 1_

q. T ,. K * * \i · & U 1!6 M ". \ r ,\ ty·( %·\' :2 :2 "L 22 ZZ2 D W - A . . ,Cj (jo . ¶O q r" Ci CC' ¶O , E , , , , , ,, ,,,0 . , ,. , V 1"" < , a r' e' ej e C|ij"Q & 'e X: ¥J "L2 T 1· ' M \ \ .j

V I , ,,. , , , , , , , AG -130' -120 -110 moo -90 -CO" 1936 12 22 (877) IjALKURE SAD 93900 LONGITUCE D IAMETER 44 KM " 0:05 '1nuj . uEFFEPERIS SOLACE - Erp !983 , N ' -8 A. 7~~ - " t' 45 .6 N ~ / V* / W

- d N * 9t §

* N -2 N \3 "4 ' ' / , / L JJ N/ " ( / " A T 3· N * "g" " ~" : 35 J'6 ^4 · ,· iZ " ""

U AgLn"y , m ^1 · "'" D 3· i? ~W " i : £ 3. g * " / A/ ,, 2·8/N 2·d N r, "/ 25 · " N / 0 / '?

'\

,-,: I I I I I 1 -125' -115 -'05 -95 -85 -75 -70°

LONG[ TLDE

EPHEI°ER[5 SOURCE - EPP 1986 ~

20

0 SI ct I

\ ~ $ " , ,;;—\-

\ \

7 X , ^_ b " tµ ,_ Iii ' ., "-V p \ F,-9 " ~ , . _a Z 7 m, I 0"

\, U u ( r" ~., CI W A' . - '7 X. , " ,i',9" """ ~. -n ~ * " ~ m ' -J % 0 Ch * 0 0 r- C" "" 0 ~ m 1j ,, ) in -Y: ' " 8 C7 < G . in cj ' c"·y \1"" "' :" ' E u ' " " _— J" &' SAD 159042 by Hypatia 1986 Dec 26 r "-'J "" {- " « X ~ ~ .> tn .J m 8P- " " C'J (S) ' '1 """ ' ' g b' Jg '$ " 8

* in , · ,'r :A" .-" _ CL < a"j — CV CJ GU _ V - -- - _ " — _ - ? ECL . 8 o A8 I_j9 " _ " CT) * CJ L

t Dm,- 0 " -'- 1^_'"""j;"-"W ' , ¶ 0 0 ,. " . __/ Y' " _ R DI "2 +;aE< --- -- '

tn , —erm " tn u7 in u7 tn SAD 77917 by Sylvia 1986 Dec 28

.8 1 |%I :¥\ 2I :1 h7:I :. 1 "%\ 'P?kT

,j<[p-—p— :jauj 1986 12 30 (946) PQESIA SAD C0322 d [afeter qe km - O:'!j4 55" ?Q jV '? 0 A, U Q 4, 'n ,1,< 2·"jj N /k I '

K i aE4 / " P" / i /A , / ~ ' , I "C: ,, " ' h " / · , : · 7 N r 0 * "? M e 3(j· ~> , / k ' ej * : L >> "" e / · # A 'V Gq {j/ / T ,, " %^ : 35 Q jg , /& x/ · , ' , ' °' ' '/ '\; ' I " Nt / , P" \ « t _0' " lV i' ' G , , \/ " "a 50 Qc? Al · ' / / ~I _ ""'& n

m " _° ' .S:"" "" ' ~ ~ 0 ~' \ I / I 0 ' ' '" , \, ,·-1' ,· ;J I I m_r~"r Q / / / "' "

i ' ,0 D · sa / d 1 I I I ° I I I I S -125° -I 15 -105 -95 -85 -75 -65°

m LONG 1TUDE

SAD 80322 by Poesia 1986 Dec 30 EPHEIER IS SOURCE - Erp !984