Asteroid Family Associations of Active Asteroids
Asteroid Family Associations of Active Asteroids
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DOI：
10.3847/1538-3881/aaa5a2
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发表时间：
2018-02-01
影响因子：
5.3
通讯作者：
Brasser, Ramon
中科院分区：
文献类型：
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作者：
Hsieh, Henry H.;Novakovic, Bojan;Brasser, Ramon
我们报告的结果，系统搜索相关的小行星家族的所有已知的活动小行星。我们发现，12颗主带彗星（MBC）中有10颗和7颗被破坏的小行星中有5颗与已知或候选家族有关，概率分别为0.1%和6%，因为主小行星带中小行星的整体家族关联率为37%。我们发现了238 P/Read和候选Gorchakov家族，311 P/PANSTARRS和候选Behrens家族，324 P/La Sagra和Alauda家族，354 P/LINEAR和Baptistina家族，P/2013 R3-B之间先前未确定的家族关联。（Catalina-PANSTARRS）和曼德拉草家族，P/2015 X6（PANSTARRS）和Aeolia家族，P/2016 G1（PANSTARRS）和Adeona家族，以及P/2016 J1-A/B（PANSTARRS）和Theobalda家族。所有与家族有关联的MBC都属于包含原始分类学分类和低平均已报告过度的小行星家族（（p）/bar（v）小于或接近0.10），而与家族有关联的破裂小行星属于包含分类学类型范围更广的小行星家族，平均已报告过度（0.06（p）/bar（v）< 0.25）。这些发现与MBC活性与组成密切相关（即，一个物体是否可能含有冰），而中断的小行星活动对成分不那么敏感。鉴于我们的研究结果，我们描述了一系列的过程，通过这些过程，年轻的小行星家族的形成可能会导致当今MBC的产生。
We report on the results of a systematic search for associated asteroid families for all active asteroids known to date. We find that 10 out of 12 main-belt comets (MBCs) and five out of seven disrupted asteroids are linked with known or candidate families, rates that have similar to 0.1% and similar to 6% probabilities, respectively, of occurring by chance, given the overall family association rate of 37% for asteroids in the main asteroid belt. We find previously unidentified family associations between 238P/Read and the candidate Gorchakov family, 311P/PANSTARRS and the candidate Behrens family, 324P/La Sagra and the Alauda family, 354P/LINEAR and the Baptistina family, P/2013 R3-B (Catalina-PANSTARRS) and the Mandragora family, P/2015 X6 (PANSTARRS) and the Aeolia family, P/2016 G1 (PANSTARRS) and the Adeona family, and P/2016 J1-A/B (PANSTARRS) and the Theobalda family. All MBCs with family associations belong to families that contain asteroids with primitive taxonomic classifications and low average reported albedos ((p) over bar (v) less than or similar to 0.10), while disrupted asteroids with family associations belong to families that contain asteroids that span wider ranges of taxonomic types and average reported albedos (0.06 (p) over bar (v) < 0.25). These findings are consistent with MBC activity being closely correlated to composition (i.e., whether an object is likely to contain ice), while disrupted asteroid activity is not as sensitive to composition. Given our results, we describe a sequence of processes by which the formation of young asteroid families could lead to the production of present-day MBCs.