Astronomy and Astrophysics – Astrophysics
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21812207c&link_type=abstract
American Astronomical Society, AAS Meeting #218, #122.07; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astrophysics
Scientific paper
We use the BSE code (Binary Stellar Evolution) of Hurley et al. (2002) to explore the binary formation channels of subdwarf B (sdB) stars, varying parameters that control mass and angular momentum loss from the system, whether or not mass transfer is stable, common envelope ejection efficiency, and the helium ignition point. 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 is produced. Sampling our database of simulations uniformly in time, we estimate the "present-day" distribution of sdB binaries with non-degenerate companions. We find that the distributions of periods and companion masses are extremely sensitive to changes in these parameters, and that reproducing the results of previous binary population synthesis studies related to hot subdwarfs requires modifying many assumptions hardwired into BSE. Our models suggest that observations of sdB-F dwarf binaries can constrain the critical mass ratio for stable mass transfer from red giants or α_CE.
Partial Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number TM8-9007X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060, with additional support from NASA grant NNX09AC83G.
Clausen Drew R.
Kopparapu Ravi Kumar
O'Shaughnessy Richard
Wade Richard A.
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