The Slow Merger of Massive Stars

Details The Slow Merger of Massive Stars The Slow Merger of Massive Stars

2002-10-16

arxiv.org/abs/astro-ph/0210368v1

Astronomy and Astrophysics

Astrophysics

4 pages, 1 figure, proc. ESO/MPA/MPE Workshop "From Twilight to Highlight: The Physics of Supernovae"

Scientific paper

10.1007/10828549_3

We study the complete merger of two massive stars inside a common envelope and the subsequent evolution of the merger product, 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 last two cases, the He abundance in the envelope is increased drastically, but significant s-processing is mainly expected in the ``explosive merger'' case.

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