The oscillations and stability of magnetized accretion discs

Details The oscillations and stability of magnetized accretion discs The oscillations and stability of magnetized accretion discs

May 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.274..171c&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 274, Issue 1, pp. 171-207.

Astronomy and Astrophysics

Astronomy

5

Accretion, Accretion Discs, Instabilities, Mhd

Scientific paper

The modes of oscillation and instability of linearized, axisymmetric and non-axisymmetric disturbances in magnetized, annular differentially rotating flows, appropriate to accretion discs, are studied. It is assumed that the fluid is incompressible and homogeneous to enable the study to focus on the interaction of vertical and toroidal magnetic fields with the sheared flow. Sufficient conditions for stability are found for non-axisymmetric modes. A heuristic derivation of a sufficient condition for axisymmetric stability is made when only toroidal fields are present. It is shown that the growth rate of the instability for almost all modes is bounded by the strength of the magnetic fields and may vary with the vertical wavenumber and azimuthal wavenumber. There always exist modes for which the growth rates are unbounded. Wave energy and angular momentum for modes are constructed to understand how the disturbances are transported. The normal-mode spectrum is computed, including the possible growth rates. The evolution of linear axisymmetric and non-axisymmetric perturbations is then studied as an initial-value problem.

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