After the Supernova: Runaway Stars and Massive X-ray Binary Populations with Metallicity

Details After the Supernova: Runaway Stars and Massive X-ray Binary Populations with Metallicity After the Supernova: Runaway Stars and Massive X-ray Binary Populations with Metallicity

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006ap%26ss.304..279d&link_type=abstract

Astrophysics and Space Science, Volume 304, Issue 1-4, pp. 279-282

Astronomy and Astrophysics

Astrophysics

3

Stars: Early-Type, Binaries: Close, Stars: Kinematics

Scientific paper

One of the main pathways by which massive runaways are thought to be produced is by the disruption of a binary system after the supernova (SN) of one of its components. Under such a scenario, the populations of runaway stars in different phases should reflect the input binary population and its evolution. Conversely, if the system stays together after the SN, a High Mass X-Ray Binary (HMXB) may result. We present simulations exploring the behaviour of such runaway and HMXB populations with metallicity, and compare them to observations. As many as two-thirds of massive runaway stars may be produced by supernovae in binaries. Decreasing metallicity lowers the fraction of O stars which are runaway, but increases the Wolf-Rayet runaway fractions and the number of potential HMXBs.

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