The Magnetoviscous-Thermal Instability in Dilute Magnetized Astrophysical Plasmas

Details The Magnetoviscous-Thermal Instability in Dilute Magnetized Astrophysical Plasmas The Magnetoviscous-Thermal Instability in Dilute Magnetized Astrophysical Plasmas

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006sf2a.conf..161i&link_type=abstract

SF2A-2006: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics Eds.: D. Barret, F. Casoli, G.

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

The accretion of a very dilute plasma is thought to be the underlying cause of anomalously low accretion luminosity onto massive black holes such as Sagittarius A^*. In these plasmas, the ion collisional mean free path exceeds the ion Larmor radius, and the flows are destabilized when either the temperature or the angular velocity decreases outwards. The cause of this behavior is anisotropic thermal conduction and viscosity, both of which limit transport to follow magnetic field lines. These plasmas are of course also prone to the standard magnetorotational instability. We discuss the detailed physical conditions under which these magnetothermal and magnetoviscous instabilities arise.

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