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Combining asteroid models derived by lightcurve inversion with asteroidal occultation silhouettes |
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| Authors: | Josef ?urech Mikko Kaasalainen David Dunham Josef Hanuš John Talbot Brian D Warner Adrián Galád |
| Institution: | a Astronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holešovi?kách 2, CZ-18000 Prague, Czech Republic b Department of Mathematics, Tampere University of Technology, P.O. Box 553, 33101 Tampere, Finland c International Occultation Timing Association (IOTA), 3 Lupin Pl, Murrumbateman, NSW, Australia d International Occultation Timing Association (IOTA) and KinetX, Inc., 7913 Kara Ct., Greenbelt, MD 20770, USA e International Occultation Timing Association (IOTA), 623 Bell Rd., Newark, NY, USA f Euraster, 1B Cours J. Bouchard, 42000 St-Etienne, France g Occultation Section, Royal Astronomical Society of New Zealand, P.O. Box 3181, Wellington, New Zealand h Japan Occultation Information Network (JOIN), Sendai Space Hall, 2133-6 Nagatoshi, Kagoshima pref, Japan i Palmer Divide Observatory, 17955 Bakers Farm Rd., Colorado Springs, CO 80908, USA j Organ Mesa Observatory, 4438 Organ Mesa Loop, Las Cruces, NM 88011, USA k Modra Observatory, FMFI Comenius University, 842 48 Bratislava, Slovakia l Ond?ejov Observatory, AV ?R, 251 65 Ond?ejov, Czech Republic |
| Abstract: | Asteroid sizes can be directly measured by observing occultations of stars by asteroids. When there are enough observations across the path of the shadow, the asteroid’s projected silhouette can be reconstructed. Asteroid shape models derived from photometry by the lightcurve inversion method enable us to predict the orientation of an asteroid for the time of occultation. By scaling the shape model to fit the occultation chords, we can determine the asteroid size with a relative accuracy of typically ∼10%. We combine shape and spin state models of 44 asteroids (14 of them are new or updated models) with the available occultation data to derive asteroid effective diameters. In many cases, occultations allow us to reject one of two possible pole solutions that were derived from photometry. We show that by combining results obtained from lightcurve inversion with occultation timings, we can obtain unique physical models of asteroids. |
| Keywords: | Asteroids Occultations Photometry |
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