This article has an erratum: [erratum]
Volume 392, Number 2, September III 2002
|Page(s)||729 - 733|
|Section||Celestial mechanics and astrometry|
|Published online||30 August 2002|
Asteroid (216) Kleopatra
Tests of the radar-derived shape model
IMCCE, UMR CNRS 8028, Observatoire de Paris, 77 Av. Denfert Rochereau, 75014 Paris, France
2 Osservatorio Astronomico di Torino (OATo), Strada Osservatorio 20, 10025 Pino Torinese (TO), Italy
Corresponding author: D. Hestroffer, email@example.com
Accepted: 5 July 2002
The shape model of Ostro et al. ([CITE]) for (216) Kleopatra – obtained from inversion of the radar data (Hudson & Ostro [CITE]) – is compared to the high resolution interferometric observations of the HST/FGS astrometer, and additionally to observed lightcurves and stellar occultations data. It appears that the radar nominal-model, while being in global agreement with these data, doesn't adequately reproduce all of them. In particular the flattening seems to be underestimated by ~20%. The HST/FGS observations should provide valuable constraints for determining a more refined shape model, since the model obtained from the radar data alone is subject to some uncertainty. Such a refined model of Kleopatra should provide valuable insights for explaining the formation of this interesting object, and the formation and evolution of binary asteroids in general.
Key words: techniques: high angular resolution / occultations / minor planets, asteroids
© ESO, 2002
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