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Modeling He-Rich Disks in AM CVn Binaries

Published online by Cambridge University Press:  22 February 2018

T. Nagel ,
S. Dreizler ,
T. Rauch  and
K. Werner
T. Nagel
Affiliation:
Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, 72076 Tübingen, Germany (nagel@astro.uni-tuebingen.de)
S. Dreizler
Affiliation:
Universitätssternwarte Göttingen, Geismarlandstr. 11, 37083 Göttingen, Germany
T. Rauch
Affiliation:
Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, 72076 Tübingen, Germany (nagel@astro.uni-tuebingen.de) Dr-Remeis-Sternwarte Sternwartweg 7, 96049 Bamberg, Germany
K. Werner
Affiliation:
Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, 72076 Tübingen, Germany (nagel@astro.uni-tuebingen.de)

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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).

Type
The Contributed Papers
Information
International Astronomical Union Colloquium , Volume 194: Compact binaries in the galaxy and beyond , 2004 , pp. 228
Copyright
Copyright © Instituto de astronomia/revista mexicana de astronomίa y astrofίsica 2004

References

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