Population Synthesis of Hot Subdwarf Stars in Binaries

Details Population Synthesis of Hot Subdwarf Stars in Binaries Population Synthesis of Hot Subdwarf Stars in Binaries

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21541929w&link_type=abstract

American Astronomical Society, AAS Meeting #215, #419.29; Bulletin of the American Astronomical Society, Vol. 42, p.281

Physics

Scientific paper

We use the BSE code (Binary Stellar Evolution) of Hurley et al. (2002) to study the formation of hot subdwarf (sdB) stars by binary processes. In the evolutionary scenarios, formation of a hot subdwarf in a binary involves removing most of the H envelope around a He-burning core, either through mass transfer to the companion star via Roche lobe overflow (RLOF), or via mass loss in a common-envelope (CE) event. We choose a large number of plausible initial binary masses and orbital periods (M1, M2, P) by Monte Carlo and follow the evolution of each binary to determine whether an sdB star (or more than one) is produced. We present the "birth distribution" (when an sdB is formed) of orbital periods and properties of the sdBs and companion stars. Sampling our database of simulations uniformly in time, we also estimate the "present-day" distribution of sdB binaries with non-degenerate companions. We compare the latter with the results of Han et al. (2003).
This work has been partially supported by NSF Grants AST 09-08642, PHY 06-53462, and PHY 05-55615, and by NASA grants NNG05GF71G and NNX09AC83G. This work is also supported by the Center for Gravitational Wave Physics, which is supported by the National Science Foundation under cooperative agreement PHY 01-14375.

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