EDP Sciences
Free Access
Volume 370, Number 1, April IV 2001
Page(s) 311 - 319
Section The solar system
DOI https://doi.org/10.1051/0004-6361:20010191
Published online 15 April 2001

A&A 370, 311-319 (2001)
DOI: 10.1051/0004-6361:20010191

Asteroid candidates for mass determination

A. Galád

Astronomical Institute, Faculty of Mathematics, Physics and Informatics, Comenius University, Bratislava, Slovak Republic

(Received 17 July 2000 / Accepted 31 January 2001)

The first 9511 numbered asteroids are studied in terms of their mutual closest approaches and encounter velocities during the period from November 6, 1967, to September 13, 2023. Several large asteroids (diameter 200 km and above) were (will be) encountered by smaller counterparts within a distance of 0.0200 AU. Thus, they are possible candidates for mass determination by the astrometrical method. Similarly, the search for effective perturbers is extended to even smaller asteroids for the much closer separation distance of 0.0020 AU and below. Only the simplified method for evaluation of observable effects on a perturbed body is used. Asteroid masses alone are not computed here. But a stronger criterion to reveal pairs for this purpose in comparison to some specially devoted papers should compensate for the difference and act as a reliable test. The best candidates for mass determination at present are asteroids (1), (2), (4), (10), (11), (24), (52) and (65). This list may be extended by at least (29) in the next 5 years and by many others in the next two decades. Several other strong perturbers from the last three decades are not included in the list, while there is still only a limited number of (or no) precise and reliable observations of perturbed asteroids before a close encounter. It seems that a perturbation by (10) is at least as effective as that by (2) and could be included in asteroid orbit determination in the future. Except for their bulk density determinations (knowing the size), the masses of perturbers could occasionally be used to improve the precision of the computed orbit for perturbed large-numbered and unnumbered asteroids as well.

Key words: minor planets, asteroids -- astrometry -- ephemerides

Offprint request: A. Galád, galad@fmph.uniba.sk

© ESO 2001

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