Near-Contact Binary Stars
Near-Contact Binary Stars
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DOI：
10.1007/978-94-009-0679-2_20
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发表时间：
1990
期刊：
影响因子：
--
通讯作者：
J. S. Shaw
中科院分区：
文献类型：
--
作者：
J. S. Shaw
一组近距离双星被称为近接触双星。根据它们的物理特性，它们被分为两个子类：V1010蛇夫座双星和FO室女座双星。列表中的成员组，他们目前的观测状况，以及他们的物理和进化的关系W大熊座双星进行了讨论。它们光变曲线的光度不对称性（奥康奈尔效应）可以用从较大的热星星到较小的冷星星的质量转移来解释。
A group of close binary stars namednear-contact binariesis defined. They are divided according to their physical characteristics into to two subclasses: V1010 Ophiuchi binaries and FO Virginis binaries. A list of members of the group, their current observational status, and their physical and evolutionary relationship to W Ursa-Majoris binaries is discussed. The photometric asymmetries in their light curves (the O’Connell effect) are explained by mass transfer from the larger, hot star to the smaller, cool star.