The evolution of low-mass close binary systems. III - 1.50 + 0.50 solar masses: Unsteady mass loss and shrinking secondaries

Details The evolution of low-mass close binary systems. III - 1.50 + 0.50 solar masses: Unsteady mass loss and shrinking secondaries The evolution of low-mass close binary systems. III - 1.50 + 0.50 solar masses: Unsteady mass loss and shrinking secondaries

Jan 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...211..486w&link_type=abstract

Astrophysical Journal, vol. 211, Jan. 15, 1977, pt. 1, p. 486-498.

Astronomy and Astrophysics

Astrophysics

59

Eclipsing Binary Stars, Mass Transfer, Stellar Evolution, Stellar Models, Unsteady Flow, Boundary Conditions, Boundary Value Problems, Computer Techniques, Energy Absorption, Energy Distribution, Main Sequence Stars, Stellar Luminosity, Stellar Mass, Thermal Energy

Scientific paper

Calculations are presented for the evolution of a binary system containing a 1.5-solar-mass primary initially separated by 3 solar radii from a 0.5-solar-mass secondary with a very deep convective envelope. Accretion is treated in two extremes where stream effects are neglected or included spherically symmetrically in the surface boundary conditions of the accreting component. The onset and initial stages of mass transfer are described, the development of mass loss on a dynamic time scale is followed, and the manifestation of a Bath-type instability in the mass-loss rate is examined. The detailed behavior of the primary's interior during this instability is analyzed, and the evolution of the accreting secondary is traced with and without the inclusion of stream effects. The model system is discussed in terms of the origin of W UMa systems. It is concluded that most W UMa systems have always existed in the contact state and that the behavior of the model supports the theory of a fission origin for close binaries.

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