Population Synthesis Studies of Close Binary Systems Using a Variable Alpha: Dependence Upon the Evolutionary State of the Giant

Details Population Synthesis Studies of Close Binary Systems Using a Variable Alpha: Dependence Upon the Evolutionary State of the Giant Population Synthesis Studies of Close Binary Systems Using a Variable Alpha: Dependence Upon the Evolutionary State of the Giant

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.0910p&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #09.10; Bulletin of the American Astronomical Society, V

Astronomy and Astrophysics

Astronomy

Scientific paper

Common envelope (CE) evolution is believed to occur in a significant fraction of close binary stars. During this phase, sizeable amounts of mass and angular momentum may be shed from the binary as the secondary spirals toward the core of the primary and transfers orbital energy into the CE. The efficiency of this transfer is very uncertain and is parameterized by a quantity, αCE, known as the CE efficiency parameter. The majority of population synthesis calculations of close binary systems have assumed that αCE is a global constant for the entire population of binaries. In previous work, we calculated model populations of present-day, zero-age post-CE binaries (PCEBs) and cataclysmic variables (CVs) using an αCE that depended upon the mass of the secondary star. In this poster, we again calculate model populations of present-day, zero-age PCEBs and CVs, but this time using an αCE that is a function of the total mass, Mp, and/or core mass, Mc, of the primary at the onset of the CE phase.
This work was funded in part by grants from the Wisconsin Space Grant Consortium and the National Science Foundation (AST-0328484) to Marquette University.

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