Evolution of close binary systems that undergo a dynamically stable late case C mass transfer

Details Evolution of close binary systems that undergo a dynamically stable late case C mass transfer Evolution of close binary systems that undergo a dynamically stable late case C mass transfer

Apr 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...214..186p&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 214, no. 1-2, April 1989, p. 186-202.

Astronomy and Astrophysics

Astrophysics

33

Binary Stars, Magnetohydrodynamic Stability, Stellar Envelopes, Stellar Evolution, Stellar Mass Ejection, Asymptotic Giant Branch Stars, Mass Transfer, Optical Thickness, Stellar Luminosity, Symbiotic Stars

Scientific paper

Numerical simulations of binary systems during dynamically stable late case C mass tranfer show that computations of the mass transfer using standard techniques give incorrect results. A technique that accounts for the finite atmospheric scale height gives results that are qualitatively different from those obtained with standard models. Mass transfer rates of the order of 0.0001 to 0.00001 solar masses/year and a wind loss rate of about 0.00001 solar masses/year are obtained. The accretion disk that forms around the companion star is very extended and its outer parts are very cool and optically thick. The total accretion luminosity of the disk is always very small compared to the primary's luminosity.

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