| Issue |
A&A
Volume 392, Number 2, September III 2002
|
|
|---|---|---|
| Page(s) | 729 - 733 | |
| Section | Celestial mechanics and astrometry | |
| DOI | https://doi.org/10.1051/0004-6361:20021006 | |
| Published online | 30 August 2002 | |
Research Note
Asteroid (216) Kleopatra
Tests of the radar-derived shape model
1
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, hestro@bdl.fr
Received:
10
April
2002
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
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.