Accretion onto main-sequence stars. I - The transient phase

Details Accretion onto main-sequence stars. I - The transient phase Accretion onto main-sequence stars. I - The transient phase

Dec 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...335..383s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 335, Dec. 1, 1988, p. 383-393. DOE-supported research.

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Computation

7

Binary Stars, Hydrodynamic Ram Effect, Main Sequence Stars, Stellar Evolution, Stellar Mass Accretion, Computational Astrophysics, Neutron Stars, Red Giant Stars, Stellar Luminosity, Thermal Boundary Layer, White Dwarf Stars

Scientific paper

A set of boundary conditions that are suitable for the study of accretion onto main-sequence stars has been derived. An important and generally neglected phenomenon is the ram pressure produced by the materials accreting onto the stellar surface. However, while important for high rates of mass accretion onto main-sequence stars, it is negligible for accretion onto both white dwarf and neutron stars. A thermal boundary condition is also provided that allows the inclusion of the accretion energy and the accretion luminosity in the evolution. These boundary conditions have been used, together with a Lagrangian, one-dimensional, hydrodynamic stellar evolution code to study mass accreting at high rates onto a main-sequence star with a mass of 1.31 solar mass, in an attempt to simulate one of the proposed scenarios for the outburst of the recurrent nova RS Ophiuchi. This study is also relevant to those members of the class of symbiotic variables that are now thought to have main-sequence stars as the mass receiver in the system. It is concluded that mass accreting onto an enlarged, massive, main-sequence star cannot be responsible for the outburst of RS Oph.

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