Double core evolution. IV - The late stages of evolution of a 2-solar mass red giant with a 1-solar mass companion

Details Double core evolution. IV - The late stages of evolution of a 2-solar mass red giant with a 1-solar mass companion Double core evolution. IV - The late stages of evolution of a 2-solar mass red giant with a 1-solar mass companion

May 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...373..246t&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 373, May 20, 1991, p. 246-249.

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Binary Stars, Main Sequence Stars, Red Giant Stars, Stellar Evolution, Stellar Interiors, Stellar Mass Ejection, Computational Astrophysics, Hydrodynamic Equations, Orbit Decay, Stellar Orbits

Scientific paper

The paper reports on the results of hydrodynamical simulations of the late phase of the common envelope stage of a binary consisting of a 2-solar mass red giant and a 1-solar mass main-sequence companion. The numerical results demonstrate that sufficient energy is released from the orbit to eject the mass within the common envelope without requiring the main-sequence companion to spiral into the white dwarf core of the red giant star. At the end of the simulation the orbital decay time scale increases rapidly to more than 160 yr. The long decay time scale reflects the removal of mass from the common envelope and its subsequent spin-up to near corotation. The ratio of the orbital decay time scale to the mass-loss time scale from the common envelope increases to more than 700, and the mass contained within the common envelope decreases to about 0.01 solar mass or less. It is argued that further orbital decay will be small and that the final binary period will be 1.2 days.

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