On the evolution of interacting binaries which contain a white dwarf
N. Langer1, S.-C. Yoon1, S. Wellstein2, S. Scheithauer2
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.
The full article is available as PostScript file via anonymous ftp.
user: anonymous or ftp; Password: your e-mail address;
file: pub/nlanger/langer_etal_2002.ps (592kB uncompressed) or langer_etal_2002.ps.gz (141kB compressed).
Display full article with ghostview (local users only!)
Fetch PostScript-File (langer_etal_2002.ps, 592kB, uncompressed)
Fetch PostScript-File (langer_etal_2002.ps.gz, 141kB, compressed)