Thermomagnetic instability of a rotating magnetized plasma disk

Abstract

We analyze the stability of a thin plasma disk which is rotating around a compact astrophysical object and is embedded in the strong magnetic field of such a source. The aim of this study is the determination of a new type of unstable modes, able to replace the magneto-rotational instability profile for low beta-values and for sufficiently small scales of the perturbations, where it fails. In particular, we consider the magneto-hydrodynamical scheme including a non-zero Nernst coefficient, corresponding to first-order collisional effects. As a result, modes with imaginary frequency lead to an instability regime when the magnetic tension vanishes. Finally, we show that, even in the presence of resistive effects, it remains a good candidate to ensure the onset of a turbulent behavior in the absence of the magneto-rotational instability.

6 pages, 2 figures

References in corpus (1)

• Inconsistency in the Standard Model for Thin Accretion Disks

Cited by in corpus (5)

• Magnetorotational instability in decretion disks of critically rotating stars and the outer structure of Be and Be/X-ray disks
• Reconciling AGN-star formation, the Soltan argument, and Meier's paradox
• Thermal generation of the magnetic field in the surface layers of massive stars
• Thermo-Galvanometric Instabilities in Magnetized Plasma Disks
• Generation of magnetic fields by thermomagnetic effects in a nonuniformly rotating layer of an electrically conductive fluid