Spin Axis Pole Distribution of the Hungaria Asteroids: An Initial Look

Details Spin Axis Pole Distribution of the Hungaria Asteroids: An Initial Look Spin Axis Pole Distribution of the Hungaria Asteroids: An Initial Look

Oct 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011epsc.conf...46w&link_type=abstract

EPSC-DPS Joint Meeting 2011, held 2-7 October 2011 in Nantes, France. http://meetings.copernicus.org/epsc-dps2011, p.46

Physics

Scientific paper

The Hungaria asteroids are small (D < 13 km) inner main belt objects with high orbital inclinations (16- 34°). As such they are not subject to planetary tidal encounters and so serve as a control group for the development of theories on binary population, spin axis rate distributions, etc. involving the near-Earth asteroid population (see Warner et al. [6]). Our previous work based on the acquisition and analysis of dense lightcurves helped establish that the spin axis rate distribution of the Hungarias is similar to the NEA population, including a strong excess of slow rotators (P > 24 h), and that the percentage of binary asteroids within the two groups is also similar. Our efforts have now turned to looking at the spin axis pole distribution of the Hungarias, e.g., to determine if that distribution is isotropic or, as Slivan [5] found for the Koronis family, there are distinct "clumps" or trends within the distribution. We report on our initial analysis that is based on the combination of dense and sparse lightcurve data (see Durech et al. [1] for a discussion regarding the differences between dense and sparse data sets). So far, our analysis is inconclusive due to the fact that there are too few Hungarias with sufficient lightcurve data to determine reliable pole solutions. We conclude by discussing the reasons why this is the case and our plans to overcome this deficiency.

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