A Comparative Study of Hungaria versus NEA Binary Populations and Spin Axis Characteristics

Details A Comparative Study of Hungaria versus NEA Binary Populations and Spin Axis Characteristics A Comparative Study of Hungaria versus NEA Binary Populations and Spin Axis Characteristics

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.5917w&link_type=abstract

American Astronomical Society, DPS meeting #38, #59.17; Bulletin of the American Astronomical Society, Vol. 38, p.596

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Since 1999, the Palmer Divide Observatory has been engaged in an on-going program of determining the lightcurve parameters for asteroids. Through June 2006, approximately 250 lightcurves have been analyzed and published.
For the last two years, work has concentrated on the Hungaria group for several reasons: the Hungarias are inner main-belt objects with generally high albedos, making them among the brightest-for-size MBAs that can be studied from Earth. A sampling of the Hungarias allows comparisons of non-planet crossing asteroids of about the same size as members of the NEA population, such as spin axis properties and binary population. Those comparisons can help determine the role of planetary tidal and YORP forces in the development and evolution of binary asteroids.
As of July 2006, the lightcurves of about 68 Hungarias have been determined (47 of them at PDO, or 69%). In addition, five confirmed or probable Hungaria binaries were initially discovered at PDO. Initial analysis shows that the fraction of Hungarias that are binary is about the same as NEAs, and the rotation rate statistics are similar with both fast and slow rotators. Also indicated is that the primary spin rates of Hungaria binaries seem to be a little slower than the average for NEA binaries.
Funding for this research was provided by NASA grants NNG06GI32G and NNX06AB30G and by National Science Foundation grant AST-0607505.

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