Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1977
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...211..881w&link_type=abstract
Astrophysical Journal, Part 1, vol. 211, Feb. 1, 1977, p. 881-889.
Astronomy and Astrophysics
Astrophysics
22
Binary Stars, Mass Transfer, Stellar Evolution, Stellar Mass, Angular Momentum, Convective Flow, Main Sequence Stars, Roche Limit, Stellar Envelopes, Stellar Luminosity, Variable Stars
Scientific paper
The evolution of both components of a 0.80 + 0.40 solar mass binary with initial separation of 1.60 solar radii is presented. This system reaches mass transfer during core hydrogen burning in the primary. The primary has such a deep convective envelope that mass transfer proceeds on a dynamical time scale. Mass exchange is followed through the first 0.00625 solar mass, by which time the transfer rate has reached 0.000833 solar mass/year. It is shown that mass transfer on a dynamical time scale leads to supercritical accretion by the secondary component and hence is presumably accompanied by extensive mass and angular momentum losses. Stability against such rapid mass transfer may impose severe limitations on the masses and mass ratios of cataclysmic variables.
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