The Minor Planet Bulletin BULLETIN OF THE MINOR PLANETS SECTION OF THE ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS
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The Minor Planet Bulletin is the journal for almost all amateurs and even some professionals for publishing
asteroid photometry results, including lightcurves, H-G parameters, color indexes, and shape/spin axis models.
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Lightcurve analysis for 819 Barnardiana was performed from observations during its 2011 opposition. The synodic rotation period was found to be 66.70 ± 0.01 h and the lightcurve amplitude was 0.82 ± 0.06 mag.
Asteroid 13241 Biyo was observed at Virginio Cesarini Observatory (Italy) on 1 night in March 2011. The resulting lightcurve shows a synodic period of 2.199 ± 0.219 h and amplitude 0.99 ±0.03 mag. in the R band.
Lightcurve measurements of 2675 Tolkien from the Shed of Science, Via Capote Observatory, and Ondrejov Observatory were taken on twenty-three nights; a period of P = 1058 ± 30 hrs, A = 0.75 ± 0.1 mag were derived.
Rotation Period Determinations for 11 Parthenope, 38 Leda, 111 Ate 194 Prokne, 217 Eudora, and 224 Oceana
Synodic rotation periods and amplitudes have been found for these asteroids: 11 Parthenope 13.722 ± 0.001 h, 0.10 ± 0.02 mag with 3 maxima and minima per cycle; 38 Leda 12.834 ± 0.001 h, 0.15 ± 0.01 mag; 99 Dike 18.127 ± 0.002 h, 0.22 ± 0.02 mag; 111 Ate 22.072 ± 0.001 h, 0.12 ± 0.01 mag with an irregular lightcurve; 194 Prokne 15.679 ± 0.001 h, 0.16 ± 0.02 mag; 217 Eudroa 25.253 ± 0.002 h, 0.22 ± 0.04 mag; 224 Oceana 9.401 ± 0.001 h, 0.09 ± 0.01 mag. An alternative 18.8 hour period suggested for 224 Oceana is definitively rejected.
CCD observations of the main-belt asteroid 604 Tekmessa were recorded during the period 2010 September to December. Analysis of the lightcurve found a synodic period of P = 5.5596 ± 0.0001 h and amplitude A = 0.49 ± 0.01 mag. The phase curve referenced to mean magnitude suggests the absolute magnitude and phase slope parameter H = 9.435 ± 0.014 and G = 0.112 ± 0.013. The phase curve referenced to maximum light suggests H = 9.279 ± 0.018 and G = 0.165 ± 0.017.
Lightcurves and Spin Periods from the Wise Observatory - 2011
We consider as targets of opportunity the random asteroids traveling through the field of view of Wise Observatory's telescopes while observing other asteroids. We report here the lightcurves and period analysis of those asteroids with results that we determine to be the most secure.
Several Well-observed Asteroidal Occultations in 2010
During 2010 IOTA observers in North America reported about 190 positive observations for 106 asteroid occultation events. For several asteroids, this included observations with multiple chords. For two events, an inversion model was available. An occultation by 16 Psyche on 2010 August 21 yielded a best-fit ellipse of 235.4 x 230.4 km. On 2010 December 24, an occultation by 93 Minerva produced a best-fit ellipse of 179.4 x 133.4 km. An occultation by 96 Aegle on 2010 October 29 yielded a best-fit ellipse of 124.9 x 88.0 km. An occultation by 105 Artemis on 2010 June 24 showed a best-fit ellipse of 125.0 x 92.0 km. An occultation by 375 Ursula on 2010 December 4 produced a best-fit ellipse of 125.0 km x 135.0 km. Of note are two events not summarized in this article. On 2010 August 31, an occultation by 695 Bella yielded a new double star. That event will be summarized in the JDSO. Finally, on 2010 April 6, an occultation of zeta Ophiuchi by 824 Anastasia was observed by 65 observers at 69 locations. Unfortunately a large shift in the path yielded only 4 chords. Results of that event, and all the events mentioned here, can be found on the North American Asteroidal Occultation Results web page.
Lightcurves for 1965 van de Kamp and 4971 Hoshinohiroba
Asteroids 1965 van de Kamp and 4971 Hoshinohiroba were observed in 2011 February in order to create lightcurves. We found no discernible rotation period for 1965 van de Kamp with some suggestion it may be longer than 36 hours. We find a synodic rotation period of 7.7 ± 0.1 h for 4971 Hoshinohiroba.
The main-belt asteroid 6670 Wallach was observed over 3 nights between February 05, 2011 and February 11, 2011 at the Observatorio Astronomico de Mallorca (620). From the collected data we determined a synodic rotation period of 4.08 ± 0.01 h and lightcurve amplitude of about 0.80 ± 0.15 mag.
The main-belt asteroid 202 Chryseis was observed 2011 January ñ February by four observers with widely separated longitudes. The derived lightcurve has a synodic period of 23.670 ± 0.001 h and amplitude of 0.20 ± 0.02 mag.
CCD photometry observations of the Eunomia member asteroid (8369) 1991 GR were made at the Palmer Divide Observatory and Center for Solar System Studies in 2011 March. Analysis using a single period search found a synodic period of 2.7368 ± 0.0001 h and lightcurve amplitude of 0.24 ± 0.02 mag. A dual-period search found a weak secondary period (assuming a bimodal lightcurve) of 49.24 ± 0.16 h. Subtracting this period noticeably improved the RMS fit of the short-period component.
Asteroids Observed from GMARS and Sanana Observatories: 2011 April - June
Lightcurves of four asteroids were obtained from Santana Observatory and Goat Mountain Astronomical Research Station (GMARS) from 2011 April to June: 948 Jucunda, 1183 Jutta, 1775 Zimmerwald and 3492 Petra-Pepi.
Analysis of CCD photometry observations in mid-2011 of the suspected binary asteroid 1866 Sisyphus made at Lowell Observatory, Goat Mountain Astronomical Research Station (GMARS), and Palmer Divide Observatory (PDO) found two low amplitude periods of 2.40 h and 25.25 h. The shorter period is similar to that previously reported. The longer period may be due to the suspected satellite but, given the lack of mutual events (occultations and/or eclipses), the evidence is not conclusive.
Asteroid Lightcurve Analysis at the Oakley Southern Observatory: 2011 January thru April
We report lightcurve rotational periods for five taxonomic A-class asteroids observed at the Evelyn L. Egan Observatory: 246 Asporina, 289 Nenetta, 446 Aeternitas, 1600 Vyssotsky, and the Mars-crosser 1951 Lick.
Call for Lightcurves: Fast Flyby of Near-Earth Asteroid 2005 YU55
As noted in the Photometry Opportunities article (this issue), on November 8, 2011 at 23:28 UT the approximately 400-meter Ctype asteroid 2005 YU55 will pass inside the Moonís orbit at 0.0022 AU (85% of the Earth-Moon distance) and reach a brightness of V~11. Such an encounter for an asteroid of this size occurs but once every few decades and thus enables a host of exciting and novel scientific investigations.
Lightcurve Analysis of Asteroids from Leura and Kingsgrove Observatory for the Second Half of 2009 and 2010
CCD photometry observations of 3151 Talbot and 4666 Dietz were obtained at the Bigmuskie Observatory, Italy, during 2011 June and July. Analysis found a rotation period of 19.49 ± 0.01 h for 3151 Talbot and a period of 2.953 ± 0.003 h for 4666 Dietz.
We present lists of asteroid photometry opportunities for objects reaching a favorable apparition and having no or poorly-defined lightcurve parameters. Additional data on these objects will help with shape and spin axis modeling via lightcurve inversion. We also include lists of objects that will be the target of radar observations. Lightcurves for these objects can help constrain pole solutions and/or remove rotation period ambiguities that might not come from using radar data alone.
Previous observations of 53 Kalypso have not resolved a rotation period ambiguity between near 9.035 hours and twice that value. New observations very strongly support the 9.035 hour period, with amplitude 0.10 magnitudes and 3 unequal maxima and minima per cycle in the interval 2011 April-July.