Advantages and Limitations of the Bipolytrope Model for Computing the Secular Evolution of Cataclysmic Binaries

Details Advantages and Limitations of the Bipolytrope Model for Computing the Secular Evolution of Cataclysmic Binaries Advantages and Limitations of the Bipolytrope Model for Computing the Secular Evolution of Cataclysmic Binaries

Feb 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...254..213k&link_type=abstract

Astronomy and Astrophysics, Vol.254, NO. FEB(I), P. 213, 1992

Astronomy and Astrophysics

Astrophysics

42

Binaries: Close, Stars: Evolution, Novae, Cataclysmic Variables

Scientific paper

For the purpose of parameter studies of the secular evolution of cataclysmic binaries we improved and generalized the bipolytrope description for mass donors with masses ≲ 1 Msun. In this simplified model the secondary is treated as a polytrope with different indices in its radiative core and convective envelope, where in contrast to previous work the core index is now allowed to vary with the stellar mass. For quantitative investigations using this bipolytrope model it is necessary to gauge the 2 free parameters of the model against full stellar models. The specific problem to which the bipolytrope model is to be applied determines the way of calibrating. We present a detailed comparison between evolutionary sequences obtained with a full stellar evolution code and corresponding bipolytrope sequences in a calibration designed to give the best overall agreement. Apart from sequences turning on mass transfer with an initial secondary mass close to the mass where ZAMS models become fully convective the simplified bipolytrope sequences reproduce the full ones with an accuracy of better than 5%.

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