Common Envelope Evolution Redux

Details Common Envelope Evolution Redux Common Envelope Evolution Redux

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.4004w&link_type=abstract

American Astronomical Society Meeting 208, #40.04; Bulletin of the American Astronomical Society, Vol. 38, p.115

Astronomy and Astrophysics

Astronomy

Scientific paper

Common envelopes form in dynamical time scale mass exchange, when the envelope of a donor star engulfs a much denser companion, and the core of the donor plus the dense companion star spiral inward through this dissipative envelope. As conceived by Paczynski and Ostriker, this process must be responsible for the creation of short-period binaries with degenerate components, but elementary energy conservation arguments fail to account for the survival of the longer-period examples of these compact binaries. Those longer-period binaries are still allowed by angular momentum conservation, but their existence implies that major terms are missing from usual formulations of the energy budget for common envelope evolution. The most plausible missing energy term is the energy released by recombination in the common envelope. We reformulate the energy budget for common envelope evolution accordingly, and explore the consequences for the formation of short-period binaries containing white dwarf components.This work is supported in part by NSF grant AST 0406726 to the University of Illinois.

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