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Studies for slowly rotating asteroids (168) Sibylla and (346) Hermentaria

Published online by Cambridge University Press:  01 March 2016

Xiaobin Wang ,
Karri Muinonen ,
Xianming L. Han  and
Chi-Tai Kwok
Xiaobin Wang
Affiliation:
Yunnan Observatories, CAS, China P.O. Box 110, Kunming 650011, Yunnan Province, China email: wangxb@ynao.ac.cn Key laboratory for the structure and evolution of celestial objects, CAS, Kunming 650011, China
Karri Muinonen
Affiliation:
Department of Physics, University of Helsinki, Gustaf Hällströmin katu 2a, P.O. Box 64, FI-00014 U. Helsinki, Finland email: karri.muinonen.@helsinki.fi Finnish Geospatial Research Institute, Geodeetinrinne 2, FI-02430 Masala, Finland
Xianming L. Han
Affiliation:
Department of Physics and Astronomy, Butler University Indianapolis, IN, United States email: xhan@butler.edu
Chi-Tai Kwok
Affiliation:
Ho Koon Nature Education Cum Astronomical Centre, Sik Sik Yuen, Hong Kong, China
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Abstract

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Studies for spin parameters and shapes of asteroids provide us with important information about the interior structure of asteroids and the physical processes they have undergone. A large sample of basic physical parameters can help us also understand the evolution of asteroids. There is scarce information for slowly-rotating larger asteroids because more effort is required for observing them. Because of this, we have established an international collaboration to study slowly-rotating asteroids. As the first step of this project, we have observed asteroids (168) Sibylla and (346) Hermentaria in 2014 and 2015 using several telescopes located in China, Chile, and U.S.A. Combining previous photometric data with our new data, we have performed preliminary analyses and obtained spin parameters and shapes with their uncertainties for these two slowly-rotating asteroids for the first time, using the convex inversion method and the virtual photometry Monte Carlo method. A pair of pole solutions for (168) Sibylla are found around (4.3°, 53.5°) and (183.5°, 52.6°) with a period of 47.0000 h. We have found that the shape of Sibylla resembles an oblate spheroid. For (346) Hermentaria, we have also found a pair of pole solutions around (134.5°, 16.7°) and (321.5°, 14.5°) with comparable rms-values with a spin period of about 17.79000 h, and a shape resembling a prolate spheroid.

Keywords

Minor planetsasteroidssolar system: generalradiative transferscatteringmethods: data analysismethods: numericalmethods: statisticaltechniques: photometric
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S318: Asteroids: New Observations, New Models , August 2015 , pp. 185 - 192
Copyright
Copyright © International Astronomical Union 2016 

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