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Instabilities in dwarf nova accretion disks

  • E. Meyer-Hofmeister
Conference paper
Part of the Astrophysics and Space Science Library book series (ASSL, volume 156)

Abstract

The dwarf novae are close binary stars where the Roche lobe filling companion transfers mass to a white dwarf. Due to the high angular momentum of the overflowing material the gas cannot fall directly onto the compact object and an accretion disk is formed. The companion star is usually a low mass main sequence star. These binary systems are very common, well documented by observations in the optical wavelength region since a long time. These objects are therefore particularly well suited to study properties of accretion disks.

Keywords

Accretion Disk White Dwarf Companion Star Stefan Boltzmann Constant High Angular Momentum 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Kluwer Academic Publishers 1989

Authors and Affiliations

  • E. Meyer-Hofmeister
    • 1
  1. 1.Max-Planck-Institut für Physik und AstrophysikInstitut für AstrophysikGarchingGermany

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