Parker's instability and viscosity in quiescent cataclysmic variable discs

Details Parker's instability and viscosity in quiescent cataclysmic variable discs Parker's instability and viscosity in quiescent cataclysmic variable discs

Mar 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997mnras.286..104r&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 286, Issue 1, pp. 104-114.

Astronomy and Astrophysics

Astronomy

4

Accretion, Accretion Discs, Instabilities, Mhd, Binaries: General, Novae, Cataclysmic Variables

Scientific paper

Reduced ionization in quiescent cataclysmic variable discs has been suggested as a possible explanation for dwarf nova outbursts. It has been shown that a self-consistent magnetic dynamo can operate in a fully ionized accretion disc and so provide an effective (magnetic) viscosity. The growth rate of Parker's instability (magnetic buoyancy) in partially ionized media is calculated along with the dispersion relation. Combined with the Balbus-Hawley instability in a similar medium, magnetic reconnection and the dynamo model are generalized for partially ionized discs. It is found that the Shakura-Sunyaev viscosity parameter does not decrease for moderately low ionization fractions typical of the discs of cataclysmic variables in the quiescent phase.

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