Nonspherical Effects in the Evolution of Close Binary Stars

Details Nonspherical Effects in the Evolution of Close Binary Stars Nonspherical Effects in the Evolution of Close Binary Stars

Aug 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005jrasc..99r.128d&link_type=abstract

Journal of the Royal Astronomical Society of Canada, Vol. 99, No. 4, p.128

Astronomy and Astrophysics

Astronomy

Scientific paper

2-D stellar evolution sequences have been calculated to assess the applicability of the assumptions traditionally made in 1-D calculations for the evolution of close binaries. The companion in the 2-D calculations is assumed to be a gravitational point source. These calculations are performed from the ZAMS to very close to when mass transfer would begin. We find that the interior properties of the models, such as the time history of the central temperature, central density, and convective core mass are essentially unchanged in the 2-D models from the 1- D results. This is true even though the convective core is not quite spherically symmetric, but slightly elongated in the direction of the companion. We treat the 2-D model surface as an equipotential. The surface matches that of a Roche potential closely until the elongation toward the companion is close to that required for mass transfer. Moreover, the surface evolution as Roche lobe overflow is approached becomes so rapid that the surface may not be able to adjust sufficiently fast to remain an equipotential. We conclude the 1-D approach is satisfactory through the events covered by our calculations except possibly just before mass transfer begins.

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