On the evolution of interacting binaries which contain a white dwarf

Details On the evolution of interacting binaries which contain a white dwarf On the evolution of interacting binaries which contain a white dwarf

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aspc..261..252l&link_type=abstract

The Physics of Cataclysmic Variables and Related Objects, ASP Conference Proceedings, Vol. 261. Edited by B. T. Gänsicke, K. Beu

Physics

7

Scientific paper

We discuss the evolution of white dwarf containing binaries, in particular such systems consisting of a white dwarf and a main sequence star which have the potential to produce a Type Ia supernova. After investigating current problems in connecting observations of supersoft X-ray sources with such systems, we consider two major problems which theoretical models encounter to produce Chandrasekhar-mass white dwarfs: the helium shell burning instability and the white dwarf spin-up. We conclude by suggesting that the formation of Chandrasekhar-mass white dwarfs may be easier when these two problem are considered simultaneously.

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