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Modeling He-Rich Disks in AM CVn Binaries

  • T. Nagel (a1), S. Dreizler (a2), T. Rauch (a1) (a3) and K. Werner (a1)

Extract

We have developed a new code for the calculation of synthetic spectra and vertical structures of accretion disks in cataclysmic variables and compact X-ray binaries. Here we present results for the CV system AM CVn.

AM CVn stars are a special type of cataclysmic variables, also called helium cataclysmics. They are systems of interacting binary white dwarfs, consisting of a degenerate C-O white dwarf primary and a low mass semi-degenerate secondary. The secondary loses mass, almost, pure helium, to the primary, forming an accretion disk. They have all in common a helium-rich composition, analoguous to the hydrogen-rich cataclysmic variables. They show photometric variabilities on time scales of ~ 1000s, the prototype of the class, AM CVn, e.g. exhibits a variability of ~ 18 min (Nelemans et al. 2001).

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Copyright

References

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Nasser, M.R., Solheim, J.-E. & Semionoff, D.A. 2001, A&A, 373, 222
Nelemans, G., Portegies Zwart, S.F., Verbunt, F. et al. 2001, A&A, 368, 939
Shakura, N.J., & Sunyaev, R.A. 1973, A&A, 24, 337
Werner, K. & Husfeld, D. 1985, A&A, 148, 417

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