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Magnetorotational stability in a self-consistent three dimensional axisymmetric magnetized warm plasma equilibrium with a gravitational field

Part of: Focus on Plasma Astrophysics

Published online by Cambridge University Press:  17 October 2016

Peter J. Catto  and
Sergei I. Krasheninnikov
Peter J. Catto*
Affiliation:
Plasma Science and Fusion Center, MIT, Cambridge, MA 02139, USA
Sergei I. Krasheninnikov
Affiliation:
Mechanical and Aerospace Engineering, University of California at San Diego, La Jolla, CA 92093, USA
*
†Email address for correspondence: [email protected]
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Abstract

Magnetorotational stability is revisited for self-consistent three-dimensional magnetized hot plasma equilibria in a gravitational field. The eikonal analysis presented finds that magnetorotational stability analysis must be performed with some care to retain compressibility and density gradient effects, and departures from strict Keplerian motion. Indeed, retaining these effects highlights differences between the magnetorotational instability found in the absence of gravity (Velikhov, Sov. Phys. JETP, vol. 36, 1959, pp. 995–998) and that found the presence of gravity (Balbus & Hawley, Astrophys. J., vol. 376, 1991, pp. 214–222). In the non-gravitational case, compressibility and density variation alter the stability condition, while these effects only enter for departures from strict Keplerian motion in a gravitational field. The conditions for instability are made more precise by employing recent magnetized equilibrium results (Catto et al., J. Plasma Phys., vol. 81, 2015, 515810603), rather than employing a hydrodynamic equilibrium. We focus on the stability of the $\unicode[STIX]{x1D6FD}>1$ limit for which equilibria were found in the absence of a toroidal magnetic field, where $\unicode[STIX]{x1D6FD}=$  plasma/magnetic pressure.

Keywords

astrophysical plasmasplasma instabilities
Type
Research Article
Information
Journal of Plasma Physics , Volume 82 , Issue 5 , October 2016 , 905820506
Copyright
© Cambridge University Press 2016 

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