The slow merger of massive stars

被引：37

作者：

Ivanova, N ^{[1
]}

Podsiadlowski, P ^{[1
]}

机构：

[1] Northwestern Univ, Evanston, IL 60209 USA

来源：

FROM TWILIGHT TO HIGHLIGHT: THE PHYSICS OF SUPERNOVAE | 2003年

关键词：

D O I：

10.1007/10828549_3

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We study the complete merger of two massive stars inside a common envelope and the subsequent evolution of the merger products a rapidly rotating massive supergiant. Three qualitatively different types of mergers have been identified and investigated in detail, and the post-merger evolution has been followed to the immediate presupernova stage. The "quiet merger" case does not lead to significant changes in composition, and the star remains a red supergiant. In the case of a "moderate merger", the star May become a blue supergiant and end its evolution as a blue supergiant, depending on the core to total mass ratio (as may be appropriate for the progenitor of SN 1987A). In the case of the most effective "explosive merger", the merger product stays a red giant. In the last two cases, the He abundance in the envelope is increased drastically, but significant s-processing. is mainly expected in the "explosive merger" case.

引用

页码：19 / 22

页数：4