Occuttau'm@Newstener

Volume III, Number 3 March, 1983

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

FROM THE PUBLISHER Astrographic Catalog data to create a data set needed to compute extended-coverage USNO total occulta- This is the first issue of 1983. tion predictions for the lunar eclipse of june 25. Since I do not want to (or have time tO) distribute o.n.'s price is $1.40/issue, or $5.50/year (4 is- extended-coverage predictions twice during the year, sues) including first class surface mailing. Back I will not do so until either I have processed the issues through vol. 2, No. 13, still are priced at additional S.A.C. data or until after the eclipse only $1.00/issue; later issues @ $1.40. Please see (when it will not make as much difference). At the masthead for the ordering address. Air mail least, I should be able to do it in time for the shipment of o.n. back issues and subscriptions is waning-phase passages through the northern Milky Way 45¢/issue ($1.80/year) extra, outside the U.S.A., starting in August. L.- Canada, and Mexico. The versatile push-button short-wave time signal re- IOTA membership, subscription included, is $11.00/ ceiver, Timekube, no longer is being manufactured, year for residents of North America (including Mexi- and Radio Shack is selling off its supply at reduced CO) and $16.00/year for others, to cover costs of prices, as low as $17. I know of no comparable overseas air mail. European and U. K. observers product which can be purchased for even triple the should join iota/es, sending DM 20.-- to Hans-j. price; if you don't have one, now is the time to get Bode, Bartold-knaust Str. 8, 3000 Hannover 91, Ger- one (or two or more, so that other observers could man Federal Republic. borrow or buy one from you). Even the CHU Timekubes are useful, since they include a button for WWV at IOTA NEWS 10 MHz.

David W. Dunham The second printing of Robertson's Zodiacal Catalog, published as Astronomical Papers prepared For use Unfortunately, this issue is being prepared under with the American Ephemeris and Nautical Almanac, considerable time pressure, as have been most of the vol. iq, part B, has been out of print (no longer issues during the past year, mainly in order to dis- available from the Goverrment Printing Office) for tribute charts and information about potentially fa- some time, and the USNO has too few copies left for vorable asteroidal occultations which will occur distribution. Improved positions are available for near the end of March. So again, I have not had most of the stars from the XZ and Perth 70 catalogs, time to prepare articles about grazes and double so it might be useful to print a new catalog, any- stars discovered during lunar occultations. The way. IOTA probably could do this, if someone would main part of my job with Computer Sciences Corp. in- volunteer to do the computer work to produce copy in volves a contract with NASA's Goddard Space Flight some reduced format from data on magnetic tape. An- Center, to design propulsive maneuvers and trajecto- other question concern accuracy; would most (or 4~- ries for the 3rd International Sun-Earth Explorer all?) who need positions to full accuracy be satis- satellite. We are planning a complex set of lunar fied with the data on magnetic tape, so that posi- swingby maneuvers to change the orbit drastically, tions could be printed only accurately enough to lo- eventually sending the spacecraft to Comet Giacobi- cate the stars on charts? IOTA already has a publi- ni-Zinner, as described on pages 135 and 136 of this cation (and machine-readable data base) of the names February's issue of Sky and Telescope. The first of Z.C stars; perhaps a crossreference list also lunar swingby will occur on March 30, and the last giving SAD, B.C., C.D., and Aitken numbers would be one in December, so this sometimes frantic work will sufficient? occupy more of njy time than usual during the remainder of this year. This will mean that I will have a Thanks to the National Science Foundation, plans are little less time for IOTA work at a time when some progressing for observing the june 11th total solar very important occultations are occurring; some eclipse from near the edges of the path in java. things which should be done simply won't be done, Alan Fiala, USNO, will lead the effort to time the and some deadlines will not be met. I could use a contacts and record Baily's beads from locations little help, especially locally, to get some of the just inside the southern limit, while David Herald jobs done, such as the IOTA incorporation effort, and I will lead the effort at the northern limit. " which has come to a standstill lately. If you will be in java and might be interested in joining this effort to measure the solar radius, I have not had time to process more of the Southern contact me. \

If my time permits, I will try to produce material the end of the telescope tube. It is this light for a next issue of o.n. in May, but the eclipse which must be screened from the observer's eye by trip noted above could delay it until july. the use of a suitable diaphragm.

LETTER The diaphragm should have a smooth hole just smaller than the dark ring, and should be in the plane of To the Editor: the exit pupil. The size of the ring can be measured directly, or calculated by dividing the diame- In reply to the editorial coment, and in regard to ter of the primary mirror by the magnification of the elimination of errors in the Taylor method (see the telescope-eyepiece combination. The separation my article "Some Hints for Timing Occultations," o. between the eye lens and the exit pupil is best de- n. 3 (2). 34), I first would like to quote from Gor- termined by taping a soft wire to the outside of the don E. Taylor's description of his method, published eyepiece and manipulating the end of the wire until in N.A.O. Technical Note No. 29, January 1974, "The no parallax is discernible between it and the exit Visual Observation of Occultations": pupil when the magnifier is moved from side to side.

"The accuracy of the observation (using the stop If it is properly made, the diaphragm wi?1 obstruct watch method — author) is enhanced if the observer none of the light reaching the telescope from the listens to a number of seconds beats whilst visually object being studied, and under certain conditions, examining the stop-watch dial. This enables him to will extend the usefulness of the telescope by a determine the tenth or fifth of a second that the magnitude or more. For more than a quarter of a stop-watch is registering at each integral second. century, I have used pupil diaphragms when observing Having recorded the decimal of a second the observer occultations, and I can recomend their use to all stops the watch at the next convenient seconds beat. serious users of Cassegrain telescopes. He my be a few tenths of a second late, but this will not matter as he has already correctly recorded [Ed: The pupil of the eye cannot be placed quite at the decimal part of the second." the idea] location, the exit pupil of the system, if t , the diaphragm occupies that position. We would wel- According to the above, the Taylor method, practi- come a short note from someone who has solved that ~ cally, eliminates a systematic error, namely the de- problem successfully with a transfer lens.] lay, in relating the stop watch to the time signal. This is possible because the determination of the MORE ON THE OCCULTATION OF 1 VULPECULAE BY PALLAS tenth or fifth of a second can be repeated several times, until the observer believes he has found the David w. Dunham and Paul Ma1ey correct fraction of the second. However, an uncertainty of the estimate of the decimal second re- Some information about this important occultation mains, as is the case with each estimate or measure- was published in "Early Planning for the Occultation ment. In this way, the statement on errors ranain- of 1 Vulpeculae by Pa11as on 1983 May 29" in o.n. 3 ing present in measurements with the Taylor method (I) 2. An important article about the event, in- is correct. Due to the repeated reading of the cluding some material not published here, will ap- watch, this uncertainty part probably will provide pear in the May issue of Sky and Telescope. No a smaller amount than is inherent in measurwents meaningful improvement of the prediction, over the with the stop watch when using methods other than current prediction based on Sitarsky's orbit and Taylor's. For that reason, I prefer the use of the Klemola's 1982 astrometry, is expected until 6 to 3 Taylor method in cases where I time occultations weeks before the event. Updates will be included on with the stop watch. I expect that the uncertainty the usual Astroalert recorded phone message for as- in estimating the decimal part of a second with Tay- teroidal occultations, at 312,259-2376 in Chicago, lor's method will not exceed ±051 or so. IL. Starting on May 23rd, prediction updates also will be broadcast on KMV during the fourth minute of Dietmar Biittner each hour.

A SKY LIGHT STOP FOR CASSEGRAIN TELESCOPES Potential observers of the occultation are asked to _ contact regional coordinators. If they know those M. D. Overbeek planning observations from home or other fixed-site locations, they can direct observers with portable With the number of users of Cassegrain and Schmidt- equipment to other locations to give the best-possi- Cassegrain telescopes increasing, it seems appropri- ble coverage of the event. Regional coordinators ate to address the frustrating problem they experi- may in turn specify local coordinators similarly to ence when observing faint objects against a bright organize the coverage in smaller areas. Please con- background. Light by-passes the secondary mirror, tact your regional coordinator if yoy are willing to flooding the observer's eye. No amount of baffling be a local coordinator. During the few days before will eliminate such interference completely. the occultation, I will try to keep in touch with the regional coordinators to provide some overall If the telescope is pointed at the bright sky or an coordination. The regional coordinators will col- illuminated wall, and the exit pupil is examined lect observation reports for their respective re- with a magnifier, the following will be seen: a gions, determine geographical coordinates, when nec- bright circle a few millimeters across, is surround- essary, and otherwise make sure that the reports are ed by a narrow dark ring, which is surrounded, in complete before sending them to me and/or to Gordon turn, by a large, bright area. The inner circle is Taylor. As for other asteroidal occultations, the the image of the primary mirror reflected by the ILOC/IOTA lunar occultation report forms can be secondary, the dark ring is the rim of the second- used, marked "Pallas" at the top, and with no copy ary, and the surrounding bright area is the image of sent to ILOC. The addresses of the regional coordi- 47

nators listed below can be found in the 1982 Novem- IL and \d1: Berton Stevens, Rolling Meadows, IL, ber IOTA roster, so only names, cities, and phone 312,398-0562. numbers are given. Robert Millis, Lowell Observato- IA, KS, MO, and eastern NB: Robert Sandy, Kansas ry, Flagstaff, AZ, telephone 602,774-3358 or -7227 City, MO, 816,763-4606. (home) will coordinate the efforts of all observers MN, NO, and SO: Jim Fox, Afton, MN, 612,436-5843. planning to record the occultation automatically, CO, WY, and western NB: Harold Reitsema, 4795 Han- using, for example, photoelectric, television, or cock Dr., Boulder, CO 80303, 303,499-5496. photographic equipment. The regional coordinators UT: Patrick Wiggins, Salt Lake City, 801,535-7316. for visual observers are 'given below. If you live Northern CA and NY: James Van Nuland, San jose, CA, in, or plan to travel to, an area where the occulta- 408,371-1307.* tion by Pallas itself is likely to occur, please ID, MT, OR, and WA: Richard Linkletter, Bremerton, contact the regional coordinator for the area, giv- ldA, 206,479-1191. After May 26, Tom Webber, Auburn, ing your name, address, and telephone number, and KIA, will serve as backup; 206,939-5904. specifying where you plan to observe. If you are mobile, or if you want additional information, you Nearly all previously reported secondary extinctions should send the coordinator a stamped, self-ad- have occurred when the star was within an angular dressed envelope, so that he can send you a map, or distance of ten diameters of the asteroid, where its other information, specifying where you might ob- gravitational domain is strongest. Hence, we recom- serve to fill in the overall coverage. First, these mend watching the star for 16 minutes centered on "southern" coordinators are listed here; they also the time of closest approach. But be careful not to will be listed in Sky and Telescope: become too fatigued, which can cause disastrous de- lays in reacting to occultation events. Take a For FL, GA, and southern SC: Harold Povenmire, short break, if necessary, noting the start and end Indian Harbour Beach, FL, phone 305,777-]303. times of any such interruptions in observing. Be For AL, AR, LA, MS, and TN: Benny Roberts, Jackson, sure to watch the star closely from two minutes be- MS, 601,373-6244. fore to two minutes after the time of closest ap- For TX and OK: Paul Maley, 15807 Brookvilla, Hous- proach, when the occultation by pa11as will occur ton, TX 77059, phone 713,488-6871 (Maley has a lot and when the possibility of secondary occultations M_ of information to distribute; please use 37¢ postage is highest. on your SASE). For AZ and NM: Peter Manly, Tempe, AZ, 602,966-39205 Most of the information in the remainder of this ar- For southern CIt: Richard Nolthenius, Los Angeles, ticle supplwents that published in the last two is- CA, 213,392-9126 or 825-2925.* sues, or that which will appear in Sky and Telescope. For Mexico: jose dc la Herran, Apartado Postal 971, Mexico 1, D.F., Mexico, 905,550-5691. Backup phone In 1980, Keith Hege and colleagues at the Steward numbers, for Paris Pismis, U.N.A.M., Inst. of As- and Sacramento Peak Observatories revealed that tronomy, Mexico City, are 905,548-5306 or -3538. their analysis of speckle interferometric observa- For Brazil: Jorge Polman, Recife, 0812,271864 or tions of Pallas indicated a possible satellite 175 270094. km ±20 km in diameter and 750 km ±100 km from Pa1- 1as. The measured change in position angle was con- For the more northern regions, coordination will not sistent with an orbit synchronized with Pa11as' be attempted, and you do not need to contact the co- 7.88-hour rotation period. Such an object would be ordinators there, unless astrometry indicates a near the limit of detectability of last year's nega- larger-than-expected north shift or unless the oc- tive radar observations of Pa11as using the Arecibo cultation path for the "speckle" satellite is spe- dish in Puerto Rico. Speckle observations of (433) cifically predicted to pass north of the nominal re- Eros currently are being analyzed to see if the Pal- gion for the main Pa11as occultation. Hence, every- las results could be explained alternately by an one should at least listen to the updates on KMV; if elongated shape rather than a satellite. Also, im- you are in one of the northern regions, and some- provements are being made with the speckle recording thing is predicted to occur there, you should con- systws which might speed up both the observations tact the regional coordinator, as described above. and their analyses. If these are successful, the The "northern" coordinators, who will not be listed position of the possible large satellite might be in Sky and Telescope (except for M. D. Overbeek), predicted for the time of the occultation of 1 Vul- '~- are: peculae. If so, its occultation path may be predicted and included with the astrometric updates South Africa: M. D. Overbeek, Edenvale, 11,53-5447. broadcast on ldWV. Eastern Canada: David Brown, Montreal, Que., 514,481-4153. In addition to determining the detailed shape of Western Canada: Niel Lafra, Calgary, Alberta, Pa11as and checking for possible satellites, we also 403,258-3151. want to determine the brightness and distance of 1 New England: Dennis DiCicco, 60 Victoria Rd., Sud- Vulpeculae's spectroscofic companion, and the diame- bury, MA 01776, 617,443-8493. ter of the primary star. According to the 1982 Yale NY: Thomas McFaul (New York City 212,397-9201) and Bright Star Catalog, 1 Vulpeculae is a single-line Hopewell Junction 914,226-4587. spectroscopic binary with a period of 249.4 days, DC, DE, MD, NJ, eastern PA, and VA: David Dunham, projected swi-major axis (for the visible star's Silver Spring, MD, 301,585-0989. After May 26, orbit about the center of mass) of 28.7 million km, an alternate message center will be at 301,449-7170 , ___m ——— + "+ (Margaret Taibi, Temple Hills, MD). * On May 28, the coordinators for AZ, CA, NY, NM, NG and northern SC: Robert Melvin, Fayetteville, NG, and UT will be at the Riverside ATM convention at 919,588-4511. Camp Oaks, CA. For last-minute coordination for IN, KV, MI, OH, western PA, and WV: Mark A11man, Co- these states, call Peter Manly or Steve Edberg at lumbus, OH, 614,863-2422 or 412,775-2304. 714,585-9593. 48

and distance of 59 parsecs. Since lines for the though somewhat better time resolution is possible companion are not seen in the spectra, it must be at with visual observation. A break in a star trail on least two magnitudes fainter than the primary, or an unguided photograph started and stopped at pre- mag. 7 or greater. The projected primary star's cise times can result in occultation times to about semimajor axis subtends about 0:'003, which would be on-second accuracy (I Vulpeculae moves about 5" in covered in half a second in case of a central occul- this time due to earth rotation) and can detect tation by Pallas. However, the true separation be- events of slightly shorter duration, provided the tween the components is likely to be larger; since focal length is at least about BOO mm. Many astro- neither it, nor the position angle, nor the second- photographers already are equipped to make such ob ary star brightness are known currently, the nature servations, which are easier than some photographs, of the step disappearances and reappearances can not since guiding is not needed and not wanted. If the be predicted. However, telescopic visual observers field of view of your lens is less than 3.8°, you probably will see a step event at only one phase, will not be able to record over the entire 16-minute since an event involving the companion will cause period desired, and would need to repoint and take too small a drop in light to be noticed if the pri- more exposures. Be sure that one is centered on the mary is visible. The secondary star probably will critical few minutes surrounding the time of closest be visible to most telescopic observers while the approach. Useful tests of pointing and exposure can primary is behind Pa11as. If one of the secondary be made a month and a week before May 28, when moon- events is timed as well as both phases of the pri- light conditions will be similar to those for the mary's occultation, you will provide three data occultation; artificial occultations of various points to define the outline of Pa11as, not just two. lengths can be simulated by moving a piece of card- board in front of the lens. The estimated diameter of the primary star is 0!'0003, which will be covered in 0.05 seconds in jay Anderson notes that weather prospects are generally good for most of the path in late May, with on- case of a central occultation. Geometry will in- ~ % crease this to an easily noticeable 0.2 seconds for ly a minimal possibility of a large weather system an observer 17 km inside the edges of the occulta- with extensive cloudiness. Although the eastern tion path, and longer for anyone located even closer portions of the track in North America are more hu- to the edges. Fresnel diffraction of the star's mid than the western parts, the local time of the light will prolong the gradual nature of both inner- event is later at night in the east, giving convec- sion and emersion significantly, so that visual ob- tive thunderstorms which form in the afternoon more servers at even the center of the path probably will time to dissipate. Overall, the weather prospects notice that the events are not instantaneous. Visu- are slightly worse in eastern Texas and are best in al observers can make comparisons with 1 Sagittae to the desert regions of northwestern Mexico. estimate variations in 1 Vulpeculae's light due to these various causes. If the path shifts substantially south, observers living in, or willing to travel to, the Virgin Is- The Universal Times of events during this occulta- lands, Puerto Rico, the Dominican Republic, Cuba, tion should be determined accurately enough so that Brazil, and especially Mexico will be crucial for points around the limb of Pallas can be specified on providing adequate coverage of the event. Hundreds the sky plane to an accuracy of 1% or less of Pa1- of amateur and professional astronomers traveled 1as' diameter, or 5 km. In the case of a central from the U.S.A. to Mexico forthe total solar eclipse occultation, this requires a timing accuracy of half in 1970, with no problems, and Dunham crossed the a second. This may sew simple to achieve, but to border several times to successfully observe lunar do it reliably requires considerable care. We need grazing occultations and an annular eclipse during ' to stress quality as well as quantity. The results the 1970'5. On May 28th, observers will not have of an occultation of a 9th-mag. star by the asteroid to travel as far into Mexico as they did for the (88) Thisbe recently was reported in the Astronomi- 1970 total eclipse. Those traveling more than about cal journal. Twelve chords were recorded during 20 miles south of the border need a temporary tour- this 1981 October event by 3 photoelectric observers ist permit, obtainable with proof of citizenship and 9 visual observers, 6 of whom had little or no (voter registration or birth certificate is ade- previous occultation timing experience. Comparison quate) and automobile registration'. Minors not ac- .._ with the accurate photoelectric timings showed that companied by parents also need a notarized letter the average reaction time of the visual observers signed by a parent or guardian giving permission to was 1.1 second, much larger than their estimates. travel in Mexico. Mexican auto insurance for one This probably was caused by an unconscious delay in day can be purchased from numerous establishments recognizing that an event actually had occurred, just north of the border, and is highly recommended. which is a problem for relatively marginal events Equiµnent should be registered with U.S. customs be- such as this one where a quarter moon was nearby and fore crossing the border. Mexico has similar forms the star was faint. Comparison of about 200 simul- which may or may not be obtainable from a local Mex- taneous photoelectric and visual lunar occultations ican consulate, where the tourist permit also can be observed in Japan has shown that reaction times for obtained in advance. Without these, you may be de- faint stars often exceed 1 second, similar to the layed an hour or two at the border (expect some de- experience with Thisbe. This should be less of a lay in any case, since Memorial Day weekend traffic problem with a bright star like 1 Vulpeculae. Al- probably will be heavy). If telescopes and other though the Japanese never achieved reaction times equipment are packed in suitcases, you will appear less than 0.30 second, their reactions for bright to be more like a normal tourist, and will be less stars were nearly all less than 0.6 second. likely to be questioned by the Mexican authorities about unregistered scientific equipment. Photographing 1 Vulpeculae provides a relatively easy way to obtain a permanent record of the star's The circle chart shows the view of the whole sky at light variations during the observing period, al- the time of the occultation for an observer in Flor- 49

Ida; the appearance will be HJ»oNy similar for others in eastern r North America. The circle rep- el ¶ resents the horizon,''with the . ? g .. m%£j S'W'·d · . · - · 5^ ·0 , D cardinal directions indicated; % e·"q'o:e Q · 0 &,L the zenith is marked with a "+" , % , . / e"s . o:'g% "3 at the center. The 94% sunlit ° . q): "% ' .·", . i? '"o "' lj

Moon, Jupiter, Saturn, all 1st : . 1%." , % a. · . . % ,·' "Q and bid-magnitude stars, and o ' T ° m , j g § f some 3rd magnitude stars in . o O '.-"4- .·', o " m2 Ei21¥" "" ;" +, X E" . gµ strategic conste11ations. are "" d?'^q'.7,q' ,, " , n " %' . , ., > .,. . qC shown. ,This,should help eveu " ' ". 7;j~ %t,>e . . Ay those with little or no previ- .. .. " ' "" ° ? ?y,' S q' OIlS knowledge of the conste11a- "A··0 o' T, ,t8 O,¶ tjous to zer? in on the regi(?n :"O'Q' ' E: : ,?,: . "'\, a " a?," " of interest in the Sumer Tri- . V. \ 'l '"p O' · angle, marked by Vega, Deneb, ° " , " " ,. , :""%, . and Altair. Tests with inex- \.' ' " perienced observers show that star-hopping from Cyg- v ;,;e" nus scans to be the most reliable method to locate 1 (Also see the Vulpeculae. This area will be closer to the eastern figures for this horizon, shown by the dashed arc, for observers in event on pp. 67 and 68) $°v'h Arizona (and in Mexico and the Rocky Mountains). The Arizona zenith is marked with an "x" between Arcturus and the Big Dipper. The eastern horizon Vulpecula are numbered on the chart. Another star, and zenith for observers in the central time zone 1 Sagittae, lies only a third of a degree above and will be midway between those for Florida and Arizo- to the right (southeast) of 1 Vulpeculae, and is L_ na. In California, the Sumer Triangle will be even about a magnitude fainter. lower, with Altair and the Moon just rising. . . . . All potential observers should practice finMng the The rectangular area, about 20° on a side, is blown star some night before the occultation, preferably up to show all stars to about 6th magnitude, includ- while a bright moon is present. The small broken ing three stars named on the circle chart: Altair, circle marked "28" shows the moon's position 24 Beta Cygni (Albireo, the famous double star), and hours before the occultation. During the night of Zeta Aquilae. The stars shown should be easily vis- May 26-27th, the moon will be full, and close to ju- ible with binoculars and small finder scopes. The piter. Some weekend before Memorial Day weekend, a arrow near the center marks the target star, 1 Vu]- small "star party" might be held for training ob- peculae. Some other stars with Flamsteed ntmbers in servers to locate the star quickly.

PRELIMINARY REPORT OF OCCULTATIONS OBSERVED DURING cultation events by 6 observers at the Milwaukee As- THE 1982 DECEMBER 30TH TOTAL LUNAR ECLIPSE tronomical Society Observatory; Gary Wedemayer timed 39 of the occultations. At Scaggsvi11e, Maryland, David W. Dunham Craig Patterson was able to time twenty occultations using a six-inch Newtonian before low altitude pre- Thomas \A. Langhans, San Bruno, CA, timed 65 occulta- vented accurate timing at mid-totality. Even far- tions during last December 30th 's exceptionally dark ther east, Philip Dombrowski timed 5 occultations eclipse, the largest number of timings reported to with a lO-inch Newtonian at Glastonbury, Connecticut. me by one observer so far. His observations will be particularly useful since 50 of the timings were of Grazes of the 10th-magnitude star C3747 were ob- reappearances! Langhans used a 36-an Schmidt-Cass. served at both the northern and southern limits, to try to obtain an improved value for the polar diame- Also in the San Francisco Bay area, Rick Baldridge ter of the moon. Paul Maley, Houston, TX, traveled L- obtained the second largest number of timings, 55, to Kailua on the island of Hawaii, where he timed ]0 using a 16-inch Dobsonian loaned by the Peninsula occultation events during the southern graze. Wil- Astronomical Society and set up at Monte Sereno in liam Albrecht got 6 additional timings near Pahoa on the Santa Cruz Mountains. Judy Sato provided valua- the east side of the island. ble assistance by keeping track of the next occultation and writing down timings from the electronic Dick Linkletter, joe Palmer, Ted Roscoe, Dave Beck- stopwatch used by Rick. He reported that both dis- er, Tom Webber, and jere Felten traveled from the appearance and reappearance of 6.8-mag. Z.C. 1014, Seattle area to North Powder, Oregon, to observe the brightest star occulted in North America during both the northern graze of C3747 and a southern this eclipse, were gradual, lasting about a quarter graze of a 7.6-mag. star. Although the sky was of a second. Some other observers also remarked clear, wind and zero-degree tanperatures made ob- about slow events for this star. He noted that, serving quite difficult. Tape recorders were kept with a little more planning and practice, they could under jackets to keep them functioning, but this and have made perhaps twice as many timings. In nearby the wind muffled the recorded voices so that they San jose, jim Van Nuland timed 19 occultations using were virtually unintelligible. It is not yet clear an B-inch Newtonian. how much data will be salvaged from this valiant effort. Farther east, the moon was lower, but Benny Roberts was able to time 52 occultations at jackson, Missis- Oscar dc las Alas, of the Manila Weather Bureau, was sippi. Gerry Samolyk reported 92 timings of 47 qc- the most successful graze observer during this 50

eclipse. Observing with a 3-inch refractor at Bula- camera, and had reserved time on the University of can, Philippines, he timed 11 events during the Arizona's 40-inch reflector at Mt. Lemon, as well southern-limit graze of 8.2-mag. SAD 78665. Don as on the University of California's 30-inch at La- Stockbauer traveled northeast from Houston to Timp- fayette, east of San Francisco. When we had to de- son, TX, where he timed the graze of SAD 78519, as cide where to go, at noon on the 29th, the weather well as several total occultations (13 altogether). forecast for eclipse time was bleak, especially Paul Newman observed the same graze from his home in along the California coast. So we opted for Arizo- Garland, TX. na. Although the clouds thinned encouragingly in the evening, this trend stopped at midnight. When Graham Blow, director of the Occultation Section of totality began, snow started to fall, and we got no the Astronomical Society of New Zealand, estimates data. This was very disappointing, especially when that 150 occultation timings will be reported from we found out that a high-pressure area had moved in- that country, mostly from the northern part. He to California more quickly than predicted, producing made one of these, recording an occultation of a clear skies throughout most of the state for the 7th-mag. star photoelectrically during a break in eclipse. Image-intensified video recording of oc- the clouds at Mt. John Observatory on the South Is- cultations during an unusually dark eclipse could land. Gordon Herdman, Auckland, was the most suc- provide valuable accurate data on the entire lunar cessful observer there, timing 48 occultations with profile which would be especially useful for analyz- a 20-cm Schmidt-Cass. He was able to see occulta- ing total solar eclipse contact timings to determine tions of stars not included in my predictions, which variations of the solar radius. Unfortunately, this were complete through 12th magnitude. was not accomplished on December 30th, and as far as I know, Graham Blow got the only photoelectric tim- Others who have reported useful occultation timings ing (just one) during this eclipse. All of the ma- include Michael Grist, Burns, TN, - 9 timings; Phil- jor observatories in the southwestern U.S.A. where lip Steffey, Santa Monica, CA, — 7; Robert Hays, photoelectric observations were planned, including Worth, IL, — 9; Richard Nolthenius, Yosanite Valley, McOonald, Kitt peak, Lowell, and Table Mountain Ob- CA, — 5; Michael Morrow, Ewa Beach, HI, — IQ; Car- servatories, were clouded out. Unfortunately, the roll Evans, Jr., Inyokern, CA, — 9; Robert Lyons, total lunar eclipses during the next decade will not Everett, WA, — 8; and Paul Teicher, Farmingdale, NY, occur in rich Milky Way fields like the ]982 eclips- - 3. es, few of them are visible from North America, and the eclipsed moon will not be dark enough to see oc- In late December, my wife and I were visiting my cultations of 12th-mag. stars unless we are lucky parents in southern California. we had assanbled an enough to have another major volcanic eruption at image-intensifier unit for our low-light-1eve1 video the right time and latitude.

ALL ABOUT UPPING YOUR ECLIPSE OCCULTATION TALLY the article imediately following this one; the second is to use two tape recorders, one to record tim- [bn M. Stockbauer ings, the other to play back a pre-recorded tape carrying timely announcwents of the same informa- I made a special effort to time total and grazing tion you would expect from an assistant (If you use occultations during the july 6th and December 30th KMV or CHU, inter alia, to guide you in making your eclipses. What I experienced may be of value to We-recorded tape, listen to the signals by ear- those attwpting observations during eclipses in the phone, to avoid having false time references appear future. on your timing tape.). However, neither suggestion can replace the valued ability of an assistant to I think that a tape recorder should be used to re- delete those upcoming events which are beyond cur- cord observations. Since the events come fast and rent observability limits.] An assistant is also furious, stopping to read a stopwatch or write down nice to have along to ensure that the time signal is an eye-and-ear timing can result in missing events. strong, to ward off the curious, etc. I believe Also, the recorder is excellent for rapidly noting that with an assistant I could have doubled or tri- personal equations, accuracies, and any special com- pled my number of timings. ments such as slow events or steps. Of course, use fresh batteries and wear it under your coat if it is Since being flexible and receiving weather forecasts cold. Periodically throughout the eclipse, make until the last possible moment helps to ensure clear sure the recorder is still working (reels turning), skies at the observing location, many times you must and use the longest tape available to minimize the observe from a location for which you have no exact number of times you must change it; a 120-minute predictions. Applying A and B factors with a calcu- cassette would cover practically the whole eclipse, lator is a long, tedious process, and there might requiring only flipping the cassette after 60 min- not be enough time. One solution for those with ac- utes. An alarm could be set to renind you to flip cess to computers would be to obtain detailed USNO the cassette. predictions for several sites in the potential observing areas, enter the coordinates, times, and A An assistant, even one with no astronomical know- and B factors for the sites beforehand on files and ledge, is extrwely useful. The problem is this: apply the factors with a program when a definite constant referral to the predictions means missing site is chosen. If a calculator must be used, and observations while looking away from the telescope. time is running short, you may not have time to ap- If an assistant is available, the data on the next ply the factors to your entire prediction set. Ap- event can be obtained without ever looking away from ply the factors to as many events as you have time the telescope, and the data does not have to be com- for, giving priority to reappearances and higher ob- mitted to memory. I see no way around this problem servability codes [Ed: especially where large fac- if you observe alone; if you know of a way, let me tors are involved]. Say, apply the factors to all know. [Ed: Two suggestions: the first is covered by events of observability code 4 or greater, which 51

will produce from about 20 to 50 events, depending way, up to 63 timings can be stowed within a bare- on the richness of the star field. Then fill in any bones HP-41C, each to OM-second resolution; addi- long gaps with events of code 3 or less for as many tional manory permits more than 300, enough to keep events as time will permit. A programnable calcula- up with the action when star clusters are occulted tor speeds up the process and reduces the chance of during a lunar eclipse. error. Often, absent-minded observers —myself included — If you are attmpting a,graze during the eclipse, lose track of the time and miss an occultation; the don't get so wrapped up in doing totals that you alarm feature is a practical remedy. At the start don't give yourself enough time to identify the of the evening's observing run, alarms can be set to star. Since during totality, very faint stars can go off (the calculator politely beeps) a few minutes be seen near the moon, several may be near the graze before each occultation. Or, if you prefer, the star. It probably is best to locate it by the posi- calculator, by fiat of a simple program, will beep tion angle for an equatoria11y mounted scope or the at you, convert the keyboard and display to stop- vertex angle for an altazimuth mount. watch mode, load the stopwatch with the current Uni- versal Time (maintained by the Time Module's clock), I found that the best way to locate the point of a and start the stopwatch. The observer simply steps total reappearance was through the position angle. up to the eyepiece and pushes the "ENTER+" key to To try to use the star field pattern requires a very record the event. Aside from the convenience, this low power eyepiece which does not let you see stars maneuver obviates the need to synchronise the stop- as faint as with a medium power eyepiece. Also, re- watch repeatedly with time signals, thus lessening ferring to charts and studying star patterns is any additional uncertainty in the timing. time-constming, and will result in fewer observations. The position angle is quick and direct, and A novel feature is the Time Module's calibration your assistant can read it to you imnediately. A procedure: fine tuning of the crystal time base is reticle eyepiece would be best to use (see o.n. i performed via the calculator keyboard. A number — (4), 34). Even without one, I was able to locate , the so-called "accuracy factor" — is keyed in and 6~ the point of reappearance fairly accurately by slew- stored; as a result, the clock rate is adjusted by ing in right ascension and declination and estab- as much as ±0.1 percent. An occasional check lishing the orientation of the moon in the eyepiece. against time signals will attest to the clock's ex- For altazimuth scopes, all this applies, except ver- actness; otherwise a refined accuracy factor is in- tex angle is used instead of position angle. serted. After more than six months of use and some initial crystal aging, my Time Module exhibits a During the Decanber 30th eclipse, I found that it clock error of less than two seconds per month. can get uncomfortably cold, even in Texas, especially after three solid hours. I discovered that poly- One drawback, from an astronomical standpoint, is ester socks might look nice, but leave a lot to be the limited range of the clock-rate adjustment. A desired as thermal insulators. Also, I had the speed-up of about 0.3 percent — three times the max- strange experience of having a hair drier fog up imtnn allowed correction — would have enabled the further a corrector plate with only a little mois- clock to run at sidereal rate. Indeed, the HP-41C ture accumulated. It took about 5 minutes of hold- would have made an accurate, portable sidereal ing the heat on it to clear it. In the meantime, 4 clock. This wish can be fulfilled, however, with a bright stars reappeared. straightforward calculator program. By retrieving the time and date from the Time Module, and armed I think we should have more notes from other observ- with the observer's geographic longitude, the local ers about their ideas for gleaning more occultation sidereal time can be computed in only a few seconds. timings during an eclipse. With the U.S.A. going A simple program loop could update the time every through a lunar eclipse drought, we need to make second or so — the calculator, in effect, mimicking every one count. a sidereal clock.

A 'TIME CAPSULE' FOR OCCULTATION OBSERVERS Meteor watchers also will want to take the HP-47C' Time Module into the field, particularly to assist 4~- Mark Gingrich during hourly meteor counts. A simple program rou- tine — only a few lines suffice — can tally each me- A new calculator accessory has made occultation tim- teor espied with the press of a button. When the ing a little easier. Called the Hewlett-Packard hour expires, the calculator automatically stores 82182A Time Module, the approximately 3-cm-square by the count and starts anew. This leaves the observe'" l-cm plastic capsule plugs into an HP-41C programa- free to concentrate on the sky, not on bookkeeping. ble calculator, adding a stopwatch, clock, alarm, and calendar to the machine's repertoire. Undoubtedly, amateurs will dream up other applications, but prospective users might wonder how much The merging of clock features with the calculator's this newfangled contrivance costs. The Time Mod- memory and programing capability inspires a legion ule's list price is $75, although, by itself, it is of astronomical applications — some of interest to as useful as photographic film without a camera. occuitation observers. The Time Module was designed specifically for the HP-41C (or HP-41CV); retrofits are not possible with For example, take the problem of timing several other Hewlett-Packard models. Hence, for the com- events within a short interval. By executing the plete systan, the cost escalates to well over $200, "SId" comand, the calculator's keyboard and display and those who desire the stopwatch features exclu- are transformed to function as a stopwatch. A tim- sively surely will find this prohibitive. On the ing is saved automatically in its own storage regis- other hand, amateurs who relish the flexibility of a ter whenever the "ENTER+" key is depressed. In this handheld computer mated with a precision timepiece 52

won't regard the price as too extravagant. The ta, at 1!'36 N on the map in o.n. 2 (16). 232. The product, after all, is unique. It can spare us a timings were reported on IAUC No. 3747. Hube noted few of the mundane tasks we occasionally goof up in that his imiersion time was inaccurate and uncer- the shivering hours before dawn. In more ways than tain; also, since the two stations were separated by one, it is a time-saver. only 13 km relative to (690)'S motion, an accurate diameter can not be determined. However, the good OBSERVATIONS OF ASTEROIDAL AND COMETARY OCCULTATIONS agrewent with the wersion timings'implies a fairly central event, with Lowe's 156-km chord length being David 'W. Dunham only a little shorter than (690)'s TRIAD diameter of 175 km. Three of the 1982 November asteroidal occultations were successfully observed, with several chords de- (375) Ursula and SAD 55791, November 15: Klemola's termined for two of them. R. Mi11is et al. deter- Lick Observatory astrometry on November 9 indicated mined the diameter of (88) Thisbe to be 232 ±12 km a path at 0'.'71 N ±0!'06, passing from Oregon to Texas from analysis of 12 observations of the occultation on the map in o.n. 3 (I), 19, and also passing near of 9th-mag. SAD 187124 on 1981 October 7, as report- Manila in the Philippines. During the two nights ed in Astronomical journal 88 (2) 229. Three of the before the occultation, plates were taken with the observations were photoelectric and showed that the long focal length U.S. Naval Observatory 61-inch as- average reaction time of the visual observers was trometric reflector at Flagstaff, AZ, and reduced 1.1 second. Consequently, only the durations re- using numerous faint secondary reference stars whose ported by the observers could be used, but even so, positions had been determined in the system of the these were crucial for obtaining a sufficient dis- AGK3R from the large-field Lick plate taken on the tribution across the occultation path for a meaning- 9th. The resulting prediction, computed by Lowell ful diameter determination. Details are given in Observatory astronomers, was at 0:'64 n, with a scat- the article, reprints of which can be requested from ter of only a few hundredths of an arc second, in Millis at Lowell Observatory, Flagstaff, AZ 86002. virtually exact agrewent with my "AGK3" predicted path, but about a radius south of Klemola's path. Comet 198Ob (Bowell) and 15th"inag. star, 1982 Sep- Observers in Oregon, Utah, and Texas were alerted so tember 30: Brian Marsden reports in T.A.U. Circular that both the Lick and USNO predictions would be (IAUC) 3751 that KL Combes, j. Lecacheux, B. Sicar- covered. Due to the favorable astrometric and dy, Y. Zeau, T. Encrenaz, and L. Vapi11on, Observa- weather prediction, and the fact that some flights toire dc Meudon; and D. Malaise, Institut d'Astro- from Washington, DC, to Salt Lake City, UT, are rel- physique, Liege, report photoelectric observations atively inexpensive (less than to Texas), I made of a close (10,000 to 20,000 km of nucleus) approach plans to join Kimball Hansen, of Brigham Yound Uni- of Comet Bowell to a 15th-magnitude star using the versity, Provo, UT, to observe the occultation visu- l-m reflector at Pie du Midi, France. At closest ally from central Utah. Although I saw the occulta- approach, half or more of the star's light was ab- tion, from a location about 3 km west of Fillmore, sorbed. However, the next night, the same astrono- UT, I was dismayed to learn after the event that my mers reported less than 0.25 absorption of the light tape recorder had failed to record the event. Due of a 14th-mag. star when the nucleus of Comet 1981f to sub-freezing tanperatures, I kept the recorder (P/Churyumov-Gerasimenko) passed within 2000 km of under my jacket, hung from a loop of twine around my their line of sight to the star. The appulses had neck, with the microphone dangling out from the not been predicted; the observers simply monitored front of the jacket. Since ldWV reception was poor, stars in the apparent paths of the comets during the I kept the Timekube receiver on my lap, and tried to two nights to see what would happen. keep it and the microphone in a good position for recording the faint signals with one hand while I (690) Wratislavia and B.D. +24° 522, November 14: A observed. Unfortunately, a couple of minutes before moderate north shift based upon Lick Observatory as- the occultation, I accidentally bumped the switch on trometry in late August, when \dratis1avia passed the microphone to the "off" position. I recomiend close to the star, was predicted on p. 6 of o.n. 3 taking some action to avoid your having the same (I). Extensive plans were made to observe the oc- mishap. I would suggest taping the switch on your cultation from the northern U.S.A. until more Lick microphone in the "on" position, except that there Observatory astrometry on November 9 showed a much is a cogent reason for not doing so: cold-weather larger shift, 1':49 north ±0:'2. Similar to the ex- control of the "off-on" condition of the tape re- _. perience for (481) Emita on October 7, discussed in corder should be via the remote control switch (lo- o.n. 3 (I) 5, this showed that astrometry obtained cated on the microphone), whose position can be mon- when an asteroid passes close to the target star a itored easily, by the tactile sense, at any time be- few months before the occultation is not nearly as fore, during, and after the recording period. The accurate as we had hoped. During such a long time, switches on the body of the tape recorder, which can the RA. and Dec. differences of the asteroid from not be monitored after your jacket has been zipped its predicted ephweris seem to change as the dis- up, are the ones which should be taped in the "re- tance to the asteroid changes. For Emita, the dif- cord" position. It is easy to lose occultation tim- ferences were nearly inversely proportional to the ings by bumping into something, changing the posi- distance, but for Wratislavia, the differences grew tions of those inaccessible switches. Also, the mi- considerably more than in simple inverse proportion. crophone should not only be plugged into the tape The behavior undoubtedly depends on the unknown er- recorder, but the plug should be taped in place so rors of the orbital elements; problems like this that it can not be pulled out accidentally. The sean to be less frequent with the better-observed plug may be left taped pemanently, if desired, but lower-numbered minor planets. Fortunately, the oc- the tape recorder should not be stored with the body cultation by Wratislavia was observed, by Andrew switches in any of the "on" positions unless the Lowe at Ardrossan and Douglas Hube at the Devon As- batteries are ranoved. The only practical solution trophysical Observatory, both near Edmonton, Alber- is to feel the remote control switch at frequent 53

enough intervals, to insure that it has not been not permitting any useful statistical analysis, were turned off inadvertently. As it turned out, the oc- made at Agassiz Station, Harvard, MA, and at Blue cultation was nearly central at my location, which Mesa Observatory, NM, but these did not help, having was nearly in line with a successful observer in scatter even greater than the Lick result. Unfortu- Texas, so any timings I might have made would have nately, clouds and a broken computer needed for au- been largely redundant. Kimball Hansen was hampered tomatic plate measurement prevented astrometry at by thickening cirrus clouds at Oak City, about 40 km USNO-Flagstaff. So, we tried to cover the entire north of my location, but apparently was able to uncertainty range, with observers in TX and OK cov- time the star's disappeardnce. Paul Maley organized ering the southern half and those in AZ covering the a chain of 14 observers from just west of Beaumont northern half. A massive storm systm covered the to well west of Houston, TX, to bracket the southern eastern U.S.A. However, Wayne Osborn managed to re- part of the possible occultation zone. Most of them cord the occultation photoelectrically at Mt. Pleas- were defeated by clouds, but Maley, Tom Williams, ant, MI, obtaining the northernmost chord. I tried and Al Kelly successfully timed the occultation, as to contact several possible observers, with the help reported in IAUC 3751 (which, however, does not give of regional coordinators, in areas where clear skies the heights above sea level, which were all less were forecast, but this was not very successful in than 12 m). John West also timed the occultation at the middle of a weekend when I also was planning to Bryan, TX. Al] of the Texan observations were near- record the event with video equiµnent. I arranged ly central, spanning about 80 km, most with chord to use Carl Schweer's M-inch Schmidt-Cass. near lengths a little greater than the 200-km TRIAD diam- Ardmore, OK. Bad weather in Atlanta delayed my con- eter. Observers in Dallas and Ft. North covered the necting flight by over two hours, so that I arrived northern part of Klemola's uncertainty zone, but all at Schweer's observatory only 10 minutes before the had no occultation. john Cotton, Dallas, planned to occultation, insufficient for finding the star and drive south to Hi11sborough, TX, where he might have setting up the equiµnent. It did not matter, since had a short occultation. However, he stopped about the actual path was in the northern part of the un- 20 km farther north, due to a shortage of time, and certainty zone, far north of us, at about 1!'35 S on saw a miss, the closest one on the north side. As- the maps in o.n. 2 (16), 232 and 233. Peter Manly 6y . tronomers from Lowell Observatory set up three 14- organized observers around Phoenix, AZ; he success- inch Schmidt-Cass telescopes with photometers in fully timed the occultation, as did Gerald Rattley, southeastern Utah, and recorded the occultation at Gary Fi11ingham, and Scott Stiers. George Balazs two of their sites. Analysis of all the observa- saw a miss from a site north of Phoenix, limiting tions should give a fairly good diameter of Ursula's the event on the north side, while a miss also was outline, although no short chords near the limits recorded at the University of Arizona's Mt. Lennon were observed. The USNO-Flagstaff astrometry, uti- Observatory, bracketing the occultation to the lizing Lick reference stars, was extremely accurate, south. The three Lowell Observatory photoelectric apparently to within 0'.'01! This combination was teams successfully recorded the occultation at sites similarly accurate for last September's occultation near Phoenix, Florence, and Picacho, AZ. The occul- by (19) Fortuna (see o.n. 3 (I) 5) and for the 1981 tation path also crossed part of southwestern Eu- March occultation by (48) Doris reported in o.n. 2 rope. The event was recorded with video equipment (IS) 201. If we had known that the astrometry would at Pie du Midi Observatory by French astronomers, as be so accurate, we would have concentrated the ef- reported on IAUC 3746. The southermost chord cur- forts by mobile visual observers near the limits, rently known was timed by Carlos Schnabel at Barce- where they could have timed short chords to define lona, Spain. The longest chord, timed by Peter Man- Ursula's outline more accurately. We will keep this ly, was 168 km long, in good agreement with Miner- in mind for future events; this occultation taught va's TRIAD diameter of 170 km. The observed chords us some valuable astrometric and observational les- span about 110 km, so it should be possible to de- sons. termine a reasonably good diameter from the timings. Further results from this occultation, as well as (375) Ursula and SAD 55766, November 17: Klemola al- from the November 15th occultation by (375) Ursula, so measured the Lick Observatory plates of Nov. 9 to will be reported in future issues. There have been update this prediction. My calculation gave a path no reports of secondary occultations. of 0!'81 N ±0!'04, crossing Queensland. I telephoned 4~- the prediction to David Herald, but unfortunately he (14) Irene and SAD 93544, 1982 December 13: Astrom·· could not locate any observers within the predicted etry by Penhallow on December 8 gave a path at i:'i S path. ±0!'1, crossing Lima, Peru, and passing near Brasil- ia, Brazil. I sent telegrams to the Peruvian Astro- (93) Minerva and SAD 76017A, November 22: Penhal- nomical Association in Lima and to Jorge Polman in 1ow°s preliminary astrometry for this event was giv- Recife, to relay to possible Brazilian observers. en in o.n. 3 (I) 6. Predominantly cloudy skies foiled most astrometric attempts for this occulta- (59) Elpis and SAD 118599, 1983 january 19: Astrom- tion, the brightest star to be occulted by an aster- etry by Penha11ow gave a time correction of 12 min. oid in the U.S.A. since 1978 June, during the week early and a path shift of 1!'6 S ±0!'2, putting it in preceding the event. Three exposures were obtained the southeastern Pacific. The astrometry agreed at Lick Observatory on the 16th during a short break better with the EMP 1979 orbit than with the Herget in the clouds, the result for the path being 1!'45 S orbit used for the predictions. If the shift for ±0!'2. Based upon experience with Lick astrometry Elpis was the same on Feb. 21, the path of the oc- for other recent occultations, I biased the predic- cultation on that date may have crossed japan or tion O:'i farther south. Unfortunately, the scatter China. in the Lick results was unusually large, giving a total prediction uncertainty of about four diame- (52) Europa and A.C. +18° gh 8" 92, january 19: ters. Attempts to improve the prediction with fur- Klemola's astrometry for this event showed that the ther astrometry, involving only one or two exposures EMP 1982 ephmeris for Europa was better than the 54

Herget ephweris, and that the star was locat- third of the cases, the occultation shadow was predicted ed about halfway between the A.C. and Lowell to miss the earth's surface far enough so that there was positions. Overall, this gave a path off the c,n ~~c'jmc'qcvcvcvc4m~~cvm~m~~NN~~c4m© earth's surface, similar to the A.C. path '" q) co«)«)cx)u»DoDmm~m~m^aj~m©ajajmmmm~^ l- u mmmmmmmp-on—ou—an—mmmmmmmm++ shown on p. 38 of the last issue. E§ m~m~mCDC.j~LULumUjuj~mmm~~ujW 0cn =Q.a.oca.ma.Eo.wmma.Q.amcL.mococ a'no a.o-a.a.a.xExExcncnxxLuxujEu'a'uxx±xxxxzujuj2m cd cd cd cd (106) Dione and SAD 80228, january 19: Penha1- LJJ LULULjj==UjUj=LLj=LLj= =LLjUjLILjLULuujujLLj==

1ow's astrometry for this event indicated a LULU LjJX 3 uj X LULU ajo OO O O Q) qj O a) O Q) Q) a) a) OO path 0!'71 S ±0!'12, crossing Spain and Italy on m cLA^~Lnots) m e~~0 emls') G =~ m e_cjm =cq ~ O ej~wm~m~ O O_mCjO 0~0 o o— o otcnio the map cn p. 39 of the last issue. I tele- =, CO C CO ¢5_ m C e m m C m~ m C ¢¶3 m C m m 3 3 Q) Q) qj Q) a) b 3 phoned this result to the Royal Greenwich Ob- m + + + + + I t I II + + + II + I I + + + I + + + + servatory and to Hans Bode in Germany. Howev- A #RRR&Z8#2G""B2""¶b3"8R8 er, Eberhard Riedl, at Kiel, German Federal bQ m O Republic, timed a LS-second occultation =~ ~q©wu)mLc)cnm~¢~¢u")<_©u7~ocnm~mnj© starting at U.T.C. 18h 59m 4355 ±055. He used uj ~~~cncvm"© ^~^jct\cq cmo~·erLc)~cmocnbcncx)% ~ m ~ ~ ~ ~ t ~ O a 9-inch reflector at longitude 10° 07' 49!'4 = o'b—mc"j

(19) Fortuna and AGK3 +11° 201, February 3: A 6.72-second occultation was observed visually by j. Pinson with a 21-cm telescope at the Club Antares Observatory at La Seyne sur Mer, France, starting at U.T.C. jgh 24m 33S. This was consistent with a 5.3-second occultation recorded photoelectrically at CERGA'S Calern laser ranging station nearby, as reported on IAUC 3776. A secondary drop in the photoelectric record about a minute after the occultation had a very slow recovery, probably indi- cating an instrumental origin.

(52) Europa and A.C. +20° 7h 52ln 82, February 8: joe Chums telephoned me his measurements of plates he took with the Astrographic Cata- log camera at Cape Observatory, South Africa, on February 7. I predicted a 1!'7 S ±0'.'2 shift, putting the path over Cape Province, which I phoned to M. D. Overbeek. Apparently, adverse weather prevented observation of the occultation.

(346) Hermentaria and SAD 99839, 1983 February 23: Penha11ow's astrometry indicated a path shift of 1!'40 S ±0!'10, placing it over a remote section of Brazil and the south Atlantic.

MORE PLANETARY OCCULTATIONS DURING 1983

Andrew Lowe and David KL Dunham

Lowe has manually compared the SAD catalog with asteroid ephemerides generated with Kep- 1erian fomulae using the precision osculating orbital elements published in the Leningrad Ephemerldes of Minor Planets for 1983, similar to the calculations he performed to find additional asteroidal occultations during 1982 published in o.n. 2 (IS) 198. Since planetary perturbations were neglected, accurate calculations by Dunham showed that, in about a 55

little hope for an actual occultation (even a secondary 24 of the last issue which might not have been one) visible from a region inhabited by potential observ- included in Gordon Taylor's or the Lowell Ob- ers. These rejected events generally occurred early in servatory searches which formed the basis for 1983, far from the osculation epoch in September. The the list of 1983 events published in o.n. 3 searches were restricted to minor planets with diameters (I) 9. The two possible occultations were not greater than 100 km given in Dunham's list described on p. found by us, but rather by Dennis DiCicco, Sky Publishing Corporation. + Table 1 4 Table 2 Information about the events is given in the two tables in the same format as those in the main list of 1983 events in o.n. 3 (I) 9. By the time this issue of o.n. is distributed, the occultations in February will have occurred. Preprints of this article, and finder charts, have been distributed to IOTA coordinators in the possible areas of visibility. Regional maps and finder charts for upcoming events will be distributed, or published here, as appropriate. You can receive local circum- stances for these additional appulses by sending a self-addressed stamped (for those in the U.S.A.) envelope to joseph Carroll, 42)6 Queen's Way, Minnetonka, MN 55343; see o.n. 3 (I) 17 and (2) 37.

Wayne Warren provided Yale Catalog data used for the prediction of the occultations by K- (909) Ulla on Septmber 4 and by (751) Faina on October 14. When possible, the predictions here have been computed using ephwerides generated from orbital elments published by Paul Herget in the Minor Planet Circulars. For these minor planets, shifts for predictions using other sources are listed in Table 3. Predic- tions for Table 3. all of the asteroidal Ephweris Differences for 1983 events have been EPHEM computed Date M.P.#. Shift A,t. SOURCE using Len- m ingrad jul 2 68 0!'145 0.9 EMP 1982 (I.T.A.) Aug 9 144 0.015 0.5 EMP 1980 elements, Sep 2 208 0.78N 2.1 EMP 1982 usually Oct 10 247 3.68N -0.4 HERGET78 taken from Dec 14 208 0.87N -5.8 EMP 1982 the E.M.P. Dec 16 849 0.06N -0.3 EMP 1982 for 1982. New orbital elements given in the 1983 E.M.P. have been used for the occultation by (346) Hermentaria on Feb. 23. The ephemeris for h~-" Pluto published in U.S. Naval Observatory Cir- cular No. 162 has been used for our calculations.

Lowe's street address given in the November, 1982, roster is incomplete; it is 4944 Dalton Drive, Apt. 75, NJA.

Notes about individual events

Feb. 21: SAD 93351 is Couteau double star #359, with equally bright components separated by 0!'15 in p.a. 170° at discovery. Since then, these parameters probably have changed due to orbital motion. Since the separation probably will be greater than the angular diameter of Armor, observers should not expect complete disappearances of the star, but only one or two dimings by 0.7 mag. as the components are occulted individually. 56

Mar 28: Lowe assumed a diameter of 146 km for (556) %1 P Phyllis, an incorrect value which he obtained from i . ' , ; ' 0 . 0 ' 0 the list on p. 25 of the last issue. That value is 0 I. 0 = a O wrong due to a transcription error. Phyllis' diameter is unknown, but judging from its brightness, it %:.!. C,. .' :' ·. is not likely to be greater than 73 km, the value 0 0 0 " ' used for the calculations here. ': ' « " : ' . O " Apr. 2: The star is in the Toulouse Astrographic 0 ' · OZ 0 " u> , " Catalog, zone +6°, plate 14h 8m, no. 97. It is : iis : 0' . . :°. ' I ° marked "A" on the detailed A.C.-based finder chart 0 p 0 1 "0 " 0 © on p. 57. Pluto is Ycdicted to pass 2:'4 south of the star (geocentric , so there probably will not be ·." 'i D b ?0 OS \,I. ' an occultation. Su p q ' ' " t, i "· i'." .: °[ :."),°,t Apr. 4: This star is also in the Toulouse Astro- graphic Catalog, zone +6°, plate 14h gm, no. 94; the , A.C. mag. is 10.5. It is marked "B" on the A.C.- h · based finder chart on p. 57. Robert Millis, Lowell 'i ' . " d \ Observatory, identified the star in the B.D. cata- ",, " . I F ,".' : " 0 . ',0 ")' ' log, which gives 9.5 for its magnitude. Pluto is ",, @ . . predicted to pass 0!'6 north of the star (geocen- ', UJ q '

tric). Mi11is reports that recent astrometry by . '. . Klemola indicates that Pluto will pass 0!'4 north of

the star (geocentric), in which case, the occulta- . Q' , . . t tion shadow would pass a short distance above the 0 6 G ~ " M S North Pole, but the uncertainties are large enough O S + that an occultation is possible for North America Q Q E) ©60·_ X D6')~ G CF (in which case, it would be a very important event). 0 Unfortunately, other pressing cormitments did not U ° '" - 1R allow Dunham to prepare a regional map for this fe cm 0 °0 ' M m :1 event in time to be included in this issue. Accur- e " G · : I ~ H " In E ate astrometry a week or so before the occultation should enable a reasonable path prediction. An oc- · · D m cultation by Charon is not likely, since it will be , " "' " ' '6 " " "§Z north of Pluto. 0 0 '^ G ."" " " E " % q " Z O Nov. 20: The star is the eclipsing variable FT Ori- ," b . - , ! , Ct" onis. The component magnitudes are 9.7 and 9.9. O m Since the expected separation of 0!'0002 is approxi- v ¶0 E el mately the separation of the Fresnel diffraction %n : :" : %- " fringes, only good photoelectric records, with time ~I TT TT " resolution of 4 milliseconds or less, will be likely to detect the duplicity. If the occultation occurs near the time of an eclipse (which should be pre- dictable), the separation could be much less than 0!'0002, so that the duplicity would not be evident 1983 3 28 (556) R4YLL!S SAD 157659 even photoelectrically. di a"eter 73 m " 0 7(17 "|*'?'<;ij I"" '","' °'5 vi"""' ~ '07 S'; -'K,.t M, N' _ !"7J"'JJ" ^ 'Y \ > Ut ' " . ',-P.".'I / /" ;;'")JJCW"":-"'~"5'"""L. '

D \", ,J :' "' /"-<> E 35_ :t I . V 0 -,. "., . .·· . 0 '-7·-:>n 0 "jz:;. ,- , ": ,, ,," · ,,," " , -~'S3 -125" -1]5 -lW «S -85 -75 -65 -S:S -St"."

LONGITUDE

SAD 157659 by Phyllis 1983 Mar 28 EFFCERIS SCKRCE W Erp 1%2 57

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, O V O,. 7 ' ' Q QO , Q " ,y .5 _" · m , · > C Q a 3 V L Q " .9 0 e Q G J " a q · L ilk :Sr! ·5 - , I, 3 f " C , I 0/ . . Q · " ;; I · 4j_ " "· " a 0 iD 0 i I « ? W O O W ' ·' ="aTms-=-,bT-3 —¥" 4-. 3 ':c'=;j 0 , S : ;j . "4 e a " K- jj?z,::. ", . E , jl . O " (3 I " "0 · 0 " i| 0 3 D . . r . . ..CC) , . ___4_"~ ., ,r' ±:"d "-:5 E ! , ·. " I " A! . "& · ""m" —:— - 0". 0 I) "3 r}' · ' m II ' :

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0 i i . " . " " "i" " "'IijI F " "+06°"--'2851 by Pluto: ' 1983' Apr i'""4 · i ,!D ' 2:S " " " ' '" ' " 'i . "W d " e '>" ' 'I 0 , "u="11L5cr"" ' U'|l!b45" '" .". S9& , . j! , , 'A"""\i' \ .. "S! / .,~T-i:m[o 'iX =m~~ :: . " · b " .. Es-—- " - ' = - "':Kt' 0 .,. _- 00 "' .i '2 . . D ""' 'j:. ;.· - i- . / " ", jES"""" \ "\ " _ ,, _ . 2 -S . ' ° " ":" '? i _ 2 S "|t??F.--Ei"i?}"\·;k),j" \r r ' ~~ / Q ®1 " " ,e5 <'---«.:· .--"_"--" :?""1""">; / "y" ·q ' i :. " -~< · '"i ' ' \ .. .' -A ::'" 7 , " , :J ", , , ·." "" " . "9 . p- 3 %- %':=L:.:,-t 7

O O , ,& O " , ed a SAD 184174 by Peitho 1983 Apr 29 · C m \_- ',:" ;$s·:ti': - U¶ Q V " , _ M I SAD 182991 by Arachne 1983 Jun 28 QC' . aj'. . C ScoRnus ' ,? ·':i' ": .";. : " ,· , ; =T=· .·X . I U , D. · . , I, : · " :" O " " ," " t , ,/,g;i',% ,/ ·p: " S>s " 2 .et3 :· " :

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:303 '?E 29 {118) FEFT·1G %C 16'174 SAD 109852 by Leto 1983 jul 2 58

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SAD 147550 by Bruchsalia 83 Jul 12 SAD 183812 by Vibilia 1983 Aug 9 SAD 158244 by Dodona 1983 Aug 15 7g""li'B,, -,sgg= . jjW' 4 'Uy"' " '" " ft . < "'>&,.- — b - 1, , r "" ^ f- ii · _. KiTm ' " "' ' 1k- i :; : ) : » W b| .-L . ' ' ) .__——J\K OP Z "T"— ' / ' "= yy .==~~ ' ___——-1— - ' :__ · ^. ( ": 3~ —;. ^a~_—=;",;" " t , I .. ":>

IS J;," "T:"—'0 " _"= "' cr 3g L , ' t . , , , " "" u-—- " ""': ": -' iWj;µ'i' "'"='="'r SAD 78100 by Lacrimosa 1983 Sep 2 SAD 129717\))by I))"Ulla 1983 Sep 4 SAD 146920 by Kalypso 1983 Sep 9 5'3G" -F-i .I ' ""'I')'" " LX ., x ajn .m i_/! >^"<"" "' """U\< \·\! " "si^"T-[" "° "" '" ' t 'i':jZ"—_:_ '' » ",

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f SAD 94752 by Lilaea 1983 Sep 12 SAD 273064 by Bredichina 83 Sep 30 SAD 38894 by Eukrate 1983 Oct 10

Z . . . ?_ '4 · yr- — t, — --. ·1;: -=- ~ .ml" " . ^r~- ' ?SeeRz-.,·, K-;ft' ' +—\-- 'Sj ::',· 'j P""" '--'" "'E""="" "" / , ~·~ ~ W_" . p '. ' , ":"") )) ' .' ' I \ ' '~+ · t /" "" " u '""m .' ~. ' -+_' :" ,, %1~-"/\ &,I j , _ .] >L , ,. ""'""" \ kL , I"q:i"::""""":iCy --A;=' , " - J/;'jg" '~..,~1. ..: " ""¶h_m~c , ...... , ... :"': . 0 " V —._ .._0+. _— — "m"" ,' . --·""" """ "° E,. " ": -. "' Z :^Y ·--. .. +. ' 4E:L- -J"" $j")' \ ,2"'" '*T,1?" =,—=' """"' " :. P ,, J """ "" "" ""' ""m" " " ""'= --·'a—.~-·" """ ""-F":S";" "Y^""

r " _ SAQ(G CJ SAD 94339 by Sapientia 1983 Oct 10 SAD 210234 by Faina 1983 Oct 14 SAD 189672 by Athor 1983 Oct 30

. 59

1983 q 29 (118) FE[TH0 SAD 18Q]7Q the tape instead of going to a neighboring station. DIATETER ICB KM = O:'CB You also could have an assistant read the time onto :'::'<7^ 'b, the tape continuously throughout the graze. Be sure that you read out the time exactly in synchrony with the wristwatch. I think about five minutes of read- ings from the watch before and after the graze should give a good idea of the uniformity of the recording, but if you can do more it would be even better. You need to avoid a very long observing period combined with only short periods of reading 42)!:'-;):! ji, :, f from the watch. A cassette that has 30 minutes or more per side would be best for this method. While Bailey suggests a least squares fit be performed to reduce the data, I feel that an adequate method % t:" ] , L...- /"'" , -- ' "" , /<µ· , would be to play the tape back and compare it to an -'ztj'q"""':"":" "":j,t'i^" , accurate stopwatch. If the tape drifts uniformly with respect to the stopwatch, the results can be ,, "" ","' "' "'""""-"i ,'2 trusted. To detemine the quality of the recording, measure the duration of the tape with the stopwatch. For example, if the tape is from 5h ocm to 5h ISm, and the stopwatch measures this duration as jgn 155, Uy' ""' ""'"' ' ',jji1 then 605 of tape time equals 61S of stopwatch time. Starting the tape at 5h OP and the stopwatch at the 25"!>"2 I " II I I I same time, 5h Dim on the tape should read im DIS on the stopwatch, 5h 02m will read 2m 02S, etc. If the -130° -120 -110 moo -90" · graze was from 5h 09n to 5h 10m, then 5h 1Om on the LONGITUJE tape should read 1Om IDS on the stopwatch, etc. To 4- obtain absolute times, calculate the ratio of the EF+EIERIS SCURCE - Erp 1982 duration of an interval on the tape to the duration of the same interval as measured by the stopwatch. ON DIGITAL QUARTZ WRISTWATCHES AS TIME SOURCES For the above example, it is jgn ODs divided by ISm 155, or 0.9836. Start the stopwatch at the first Don M. Stockbauer whole minute of the tape and make sure the two are drifting uniformly up until the graze begins. Read I recently bought a digital quartz LCD wristwatch to the times of the graze events from the stopwatch, replace my old analog model, for about $35. I com- and when the graze ends and your wristwatch times pared it against ldWV and was quite surprised at its again are being announced, make sure the tape has unifomity and accuracy. In the course of one month drifted by the expected amount and continues to do it uniformly lost exactly one second. I believe so. Using the example above, if I start the tape at that it probably could be adjusted to even higher 5h ON and the stopwatch at the same time, and I accuracy, but the important point is that the drift call an event at 7m 1253 by the stopwatch, the true is very slow and very uniform. I believe that such time is 5h OOm + 0.9836 x 7m 1253 = 5h 07m 0552. If a watch should be a part of every graze observer's the drift shows random irregularities, the results equipment because it would be a good time source in cannot be trusted. However, I have reduced about case of complete loss of shortwave time signals. one hundred tapes since 1974, and have never encoun- [Ed: For a tuning-fork-controlled timing device, see tered a tape that did not drift evenly. Fresh bat- "Digital Electronic Timer," by T. H. Campbell, jr., teries are a must, and keeping the recorder warm un- o.n. i (7) 61. For other quartz-controlled devices, der your coat in cold weather is a must also. An see "The Danish Time-Cube," by N. P. Wieth-knudsen, external microphone ensures a good recording under a o.n. i (8) 79, and "Auditory Electronic Occultation thick coat. It would be a good idea to replace the Timer," by C. J. Bader, o.n. i (IQ) 100. For earli- wristwatch battery frequently. It would not pay to er report of use of digital watch for occultation have it die during the graze! It is best not to use m work, see "The Lacombe Graze," by F. J. Howell and any of the special functions of a multi-function F. Loehde, o.n. i (8) 78.] watch while you need the stable time base. Acci- dentally pressing a wrong combination can result in First, determine the uniformity of your watch losing the time base. against MdV. If it has a uniform, linear drift, or almost no drift, over a period of a week or so, it A final correction must be applied to convert the is good enough for this method. Record its drift in wristwatch time to UT. As close to the graze as is seconds per day. feasible, synchronize the watch with hlWV and record the time and date. Soon after you get back from the The basic method is outlined in "Some Comnents on graze, see how much the watch has drifted. If it is Reading-out Graze Tapes," by R. R. Bailey, o.n. i negligible, use the wristwatch time as UT. If it ' (8) 75. Bailey suggests that a graze observer still has drifted, calculate a correction factor to con- can obtain data if he cannot receive time signals. vert the wristwatch time to UT. If The observer goes to a neighboring station, records A = the amount of time from synchronizing the several minutes of time signals on his tape, leaves wristwatch with WldV until the graze, the tape running, and returns to his station and ob- B = the amount of time from synchronizing the serves the graze. Then he returns to the other sta- wristwatch with ldWV until rechecking against \4\AV, and tion and records several more minutes of time sig- C = the number of seconds of drift (wristwatch nals. All this applies using a wristwatch, except fast = negative, wristwatch slow = positive), that the observer reads the time from the watch onto then the factor is A x C + B , which is added alge- 60 braica11y to the times as determined before (pay at- sun, which will be at apparent Dec1. -11° 12', RA. tention to the signs). GIB gives the drift rate, 13h 4@7, 4h 34'!14 less than that of e Sagittarii, or which should match the results of your initial they can set up their telescopes the night before checkout of the watch. For example, if A = 1.0 day, the occultation, pointing them to a star with nearly B = 2.0 days, and C = -1.0 second (wristwatch ahead the same declination as e Sgtr. at a time when it 1.0 second when rechecked), the correction factor is will have the same altitude and azimuth (the amount 1¢02¢0"120 = _o2s of sidereal time will be the difference in RA.). Unfortunately, the far southern declination and rather small elongation from the sun preclude North- which, when added to the previously determined time ern-Hwisphere astrometry; during the few months be- of 5h 07m 0552, gives 5h 07m 0457. fore the event, Hispania will be even farther south. We probably will need to rely on Perth Observatory This method would work for any field time source as for the necessary astrometry, which may be difficult long as its uniformity and accuracy could be trust- due to the large magnitude difference. A trip to ed. Continued checks of my quartz wristwatch have the mid-Pacific may be worthwhile for an event much convinced me that it is more than adequate under any rarer than even a total solar eclipse. Any possible conditions, even large temperature variations. expedition plans will be announced in future issue. Like the other bright stars occulted by asteroids in PLANETARY OCCULTATION PREDICTIONS FOR 1983 1983, this is conveniently a weekend event, occurring on Saturday evening east of the International This is a continuation of the earlier articles bear- Date Line. ing on this subject (see o.n. 3 (I) 9 and o.n. 3 (2) 25 and 37). The tables list the occultations of un- Nov. 19: See note for Apr. 7, o.n. 3 (I) 19. catalogued stars found at Lowell Observatory which were not included on p. 26 of the last issue (which Dec. I: In his Bulletin 27, Gordon Taylor offers to included events only through the end of March). The compute local predictions for this occultation. The article by Mi11is, Franz, Wasserman, and Bowell bright-limb imnersion will not be observable. Even listing these events, "Occultations of Stars by So- the mersion will be difficult, since the defect of lar Systw objects. iii. A Photographic Search for illumination (width of dark crescent in p.a. oppo- Occultations of Faint Stars by Selected Asteroids," site the sun) will be only 0!'37; good atmospheric was published recently in Astronomical journal 88 seeing will be needed. (2) 236. (Text continues on page 67. )

Notes about Individual Events (continued) "Cl !<,Ly, , ' /"' ' 'J " Apr. 24: The position of the faint star to be occulted by Pluto on this date is marked "24" at the ~ edge of the A.C.-based finder chart on p. 57. :'i X LV~cj> ~ I H 'R" " ;Sr ? Apr. 26: The A.C. path crosses Mexico, as shown on '" ,7' the regional chart for this event in this issue. If ~ the shift for this event is similar to those indi- " " I)" " cated by astrometry for the occultations by Europa " E7> ~ on jan. 19 and Feb. 8, the path probably will be 0'.'9 GJ - 2 S ±0'.'4, crossing the western and south-central U.S. Z A. The other rectangles drawn on the Atlas Coeli 8 'A"" ·= i -_ y' inset for the A.C.-based finder chart for this event .J © are for occultations in February and on March 19 O.. "'?:G, - / , E shown in detail on p. 41 of the last issue. < -- I i ( 0 / _ "D 88 E" Aug. 1, (511) Davida: The star is in the USNO C-cat- ]! S P-:J u alog, number C14047, where its magnitude is given as Z El 10.9. The star is on the map of the 1982 july 6th _ J' I. _ J)",cf - , e! ) ^4" CL lunar eclipse star field in o.n. 2 (16) 217, and was A ¥ occulted by the relatively bright southern part of " ¥ " I CL the moon during the partial phases of the eclipse (D — -- a --P . / IE for observers in the eastern U.S.A.; probably nobody q" ¥ observed that occultation. " " 2 , ,L/ 8 X · . "W "" "" ,2T_ _ g a Oct. 23: SAD 210091 = e Sagittarii = FK4 689 = Kaus . Australis, the brightest star yet predicted to be S ". P' f' \ " ~ occulted by an asteroid, and with the largest occul- . tation Dm. As noted in o.n. 2 (IS), 203, an occultation of a star this bright, or brighter, by an as- " CJ teroid as large as, or larger than, (804) Hispania, ' 0'/ " " . T occurs only about once every 141 years. In the o.n. " g "'"' "' 2 (IS) article, I erred, reversing the paths computed from orbital elements given in EMP 82 and by Her- [y ., :"S' ,.: ' " O, r' If , get. Unknown to me then, astrometric observations m Cl R "CJ ' made at Lowell Observatory last February 21 reported ,,,m I _ J

1983 UNIVERSAL P L A N E T S T A R 0 CC U L T A T I 0 N El M 0 0 N Eplwneris DATE TIME NAME mv 4,AU Lowell # mv RA. (1950)Dec. e,m. Dur .d.f. P Possible Area SUN El %Sn1 UZ Source Apr 16 22h 18"-24" Interamnia 11.5 2.55 692878 10.3 13h26m2 -33°27' 1.5 23S 21 11 India, Mideast,southeast Europe 156°136° 15+ none EMP 1977 Apr 26 5 53 Europa 11.5 2.71 679863 10.6 8 12:2 21 42 1.3 15 17 14 central Canada;nw¢ra1 USA?S 86 81 99+ all HERGET78 May 5 1 12 Cybele 12.3 2.79 680214 ]1.8 20 29.6 -15 58 1.0 24 25 13 southern Africa 98 9 51- all EMP 1975 May 10 0 09 Interamnia 11.5 2.57 692719 ]0 13 08.5 -30 57 2 24 23 I] Antarctica; s. & w. Austra1ia?n 150 152 7- S 65°S EMP 1977 May 12 20 06 Hygiea 9.51.88 681123 11.7 1312.5 -]3 32 .13 57 35 6 South Africa?n 150 149 0+ none SCHMADEL jun 3 3 56-61 Patientia 11.6 2.34 680969 11.5 18 54.8 -24 27 0.8 26 28 12 SouthAfrica, AntarcticPeninsula 149 51 57- all HERGET78 Jun 8 21 08 Davida 11.8 2.82 680743 13.7 19 32.9 -20 00 0.2 3.0 30 12 western Australia 145 115 7- c112°E EMP 1982 Jun 25 18 16 Interamnia 12.0 2.97 692759 14 13 02.] -25 41 0.2 35 35 13 New Zea1and?n; Austra1ia?n 110 73 100- all EMP 1977 Jun 29 10 32-44 Cybele 11.5 2.19 680235 ]4.1 20 33.4 -15 34 .08 38 36 10 western U.S.A.; Hawaii?s 150 17 85- none EMP 1975 Jul 1 7 56-63 Davida 11.5 2.68 680759 13.0 ]9 18.3 -21 30 0.2 21 21 12 cen&w USA or Canada?s; Hawaii?s 170 56 71- e135°W EMP 1982 jul 4 2 00-19 Cybele 11.4 2.16 680239 13.0 20 31.0 -15 44 0.2 34 31 10 cen. Africa, cen. South America 155 72 44- e 25°W EMP 1975 Jul 4 4 21-29 Davida 11.5 2.68 680763 11.9 19 16.1 -21 42 0.6 21 20 12 Zaire, sc. Brazi1?n; Patagonia 174 91 43' e 55°W EMP 1982 Jul 19 12 52 Hygiea 10.4 2.58 691242 13.5 13 29.9 -13 05 .06 25 18 8 Indonesia 90 30 74+ all SCHMADEL Jul 31 4 51-58 Ceres 7.8 2.00 680439 12.4 22 02.5 -26 20 .02 84 23 3 southern Canada, U.S.A., Mexico 159 52 68- e 95°W APAENAXX Aug 1 8 23-38 Davida 11.6 2.73 680121 10.8 18 54.4 -23 37 1.3 25 24 12 Guatwla;Mex?n;NwZlnd?s;eAustr1 154 107 57- el35°W EMP 1982 Aug 13 0 07-21 Cybele 11.4 2.17 681025 13.0 20 03.6 -17 48 0.2 31 29 10 South Africa; Patagonia?n 160 101 24" W 35°W EMP 1975 Aug 17 23 58-75 Cybele 11.5 2.20 681030 12.5 20 00.7 -18 03 0.4 34 32 10 southern Africa, Patagonia 154 36 74+ W 32°E EMP 1975 Sep 3 11 36-70 Davida 12.0 3.04 680142 12.7 18 42.0 -2511 0.5101 104 13 China, Indonesia; w.Austra1ia?e 120 171 19- none EMP 1982 Sep 14 2 29 Patientia 12.4 2.87 680066 10.8 18 07.7 -29 34 1.8 30 36 15 north-central U.S.A. 101 13 50+ all HERGET78 Sep 18 17 15-42 Cybele 12.0 2.51 681048 12.8 19 53.4 -19 06 0.4130 130 12 eastern Africa 122 20 89+ all EMP 1975 Oct 4 1 31-36 Patientia 12.6 3.14 680090 11.2 18 21.3 -29 46 1.6 16 20 16 nw. South America, West Indies 85 118 8- none HERGET78 Oct 25 0 38 Cybele ]2.5 3.03 681070 12.8 20 10.6 -18 58 0.618 20 14 cen.Chile, n.Argentina, s.Brazi1 90 127 90- e 55°W EMP 1975 Nov 27 9 52 Ceres 9.1 3.04 680825 ]1.9 21 47.3 -24 12 .08 44 15 4 eastern Australia 77 166 51- none APAENAXX —— -—Table 1 is above.———— —————Table 2 is below.——— 1983 MINOR PLANET MOTION COMPARISON DATA APPARENT 1%3 5 6 (71) Nl« SAD 117178 DATE .No, NAME km-diam.-" RSOI °/Day PA. A. C. Number Shift Time R.A. Dec. DIAPETER 106 m - 0:'06 1 3h28m1 -33°37' '"" " Le,3u ,, ,? ," : , ? 'N " ,:', 1G 1 Apr 16 704 Interamnia 339 0.18 2811 0.191 294° +22° 8h08"129 -1:37 0.7 8 14:1 21 36 Apr 26 52 Europa 291 0.15 1803 0.237 98 20 31.4 -15 52 \3 May 5 65 Cybele 311 0.15 2181 0.155 74 ' . a 4, ^ "" l ^ H W May 10 704 Interamnia 339 0.18 2801 0.181 314 13 10.3 -31 08 May 12 10 Hygiea 443 0.33 3361 0.138 303 13 14.2 -13 43 Jun 3 451 Patientia 281 0.17 1976 0.152 240 18 56.8 -24 24 Jun 8 511 Davida 335 0.16 2924 0.129 243 19 34.8 -19 55 RAJ :,/ ,: ,,, ', ' , .·:c;L G " .1/ P '>

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L 680214 by Cybele 1983 May 5 SAD 117178 by Niobe 1983 May 6 SAD 204221 by Interamnia '83 May 9 67

Dec 30, (91) Aegina: Astrometry for an unobserved occultation in 1981 "2CJ' u (I) ' ty a . ' April showed a very large correction (mostly in the direction of mo- " S) e e . .% "cD , : ' tion) to the ephaneris, which has not been updated further. ,0 % JJ O Unfortunately, time did not allow checking four finder charts for po- ·19 - · "t? 0 0 0e O G) O 0 O %) CI C)QD ,

tential European events against Atlas Eclipticalis or True visual Mag- 0 €, 0 ' " ' 0 " ' Ct)QO " nitude Atlas, or for adding Atlas cocli-based large-field charts. Dc) ¢) \o415I G ' ·18 - " :· E) 4 ' D . 0 · E

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