基于TESS S1-S13观测的小行星族的旋转周期和形状非球面性
Rotation periods and shape asphericity in asteroid families based on TESS S1-S13 observations
摘要：
利用TSSYS-DR 1小行星光变曲线数据库中的9912条TESS小行星光变曲线，分析了16个主带族2859颗小行星的自转周期和光变曲线振幅的分布。我们发现，光变曲线的分布特性遵循一个家庭的特定字符在一些小行星家族，包括匈牙利，玛丽亚，朱诺，Eos，Eucharis和Alauda家庭。而在其他大家庭中，这些分布通常彼此非常相似。我们证实，老家庭往往包含更大的比例更球状，低振幅小行星。我们发现，旋转周期分布是不同的核心和外围的弗洛拉和玛丽亚家庭，而灶神星，Eos和Eunomia家庭缺乏这一功能。我们还证实，非常快速旋转的小行星接近球形（或旋转顶部形状），旋转速度低于11小时的小行星也比4- 8小时周期范围内的小行星更接近球形，预计这组包含最细长的天体。
英文摘要：
Here we present the analysis of the distribution of rotation periods and light curve amplitudes based on 2859 family asteroids in 16 Main Belt families based on 9912 TESS asteroid light curves in the TSSYS-DR1 asteroid light curve database. We found that the distribution of the light curve properties follow a family-specific character in some asteroid families, including the Hungaria, Maria, Juno, Eos, Eucharis, and Alauda families. While in other large families, these distributions are in general very similar to each other. We confirm that older families tend to contain a larger fraction of more spheroidal, low-amplitude asteroids. We found that rotation period distributions are different in the cores and outskirts of the Flora and Maria families, while the Vesta, Eos, and Eunomia families lack this feature. We also confirm that very fast spinning asteroids are close to spherical (or spinning top shapes), and minor planets rotating slower than ~11 hour are also more spherical than asteroids in the 4--8 hour period range and this group is expected to contain the most elongated bodies.
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