Ground-Based Optical Observations of Asteroids

Details Ground-Based Optical Observations of Asteroids Ground-Based Optical Observations of Asteroids

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005hia....13..752c&link_type=abstract

Highlights of Astronomy, Vol. 13, as presented at the XXVth General Assembly of the IAU - 2003 [Sydney, Australia, 13 - 26 July

Astronomy and Astrophysics

Astronomy

Scientific paper

Many physical parameters of asteroids can be inferred from remote optical measurements. Rendez-vous missions make it possible then to reliably generalize remote-sensing results to the vast majority of bodies that will never be visited by space probes. Estimates of sizes and albedos are produced by several optical techniques including Adaptive Optics Speckle Interferometry and Polarimetry. Relevant results have been obtained including the discovery of many binary systems for which mass determinations become possible. Astrometry is also used to derive the masses of the biggest asteroids through measurements of orbital deflections caused by mutual close encounters. Another major technique is Spectroscopy. Reflectance spectra provide clues about the composition of asteroid surfaces. Particularly important has been the identification of hydration features in asteroid spectra including many M-types. Spectroscopic observations of many S-type NEOs have found evidence of space-weathering phenomena nicely complementing the evidence found by the Galileo probe for Ida and Gaspra. Photometry is used to evaluate shapes and better understand asteroid internal structures. According to lightcurve evidence down to small sizes there are not objects having a spin rate beyond the fission limit. However the only one object studied by ""in situ"" measurements 433 Eros seems mostly a well consolidated body.

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