Parker-Jeans Instability of Gaseous Disks Including the Effect of Cosmic Rays

Details Parker-Jeans Instability of Gaseous Disks Including the Effect of Cosmic Rays Parker-Jeans Instability of Gaseous Disks Including the Effect of Cosmic Rays

2005-06-07

arxiv.org/abs/astro-ph/0506137v1

Astrophys.J. 636 (2005) 290-302

Astronomy and Astrophysics

Astrophysics

19pages, 14figures submitted to ApJ

Scientific paper

10.1086/498056

We use linear analysis to examine the effect of cosmic rays (CRs) on the Parker-Jeans instability of magnetized self-gravitating gaseous disks. We adopt a slab equilibrium model in which the gravity (including self-gravity) is perpendicular to the mid-plane, the magnetic field lies along the slab. CR is described as a fluid and only along magnetic field lines diffusion is considered. The linearised equations are solved numerically. The system is susceptible to Parker-Jeans instability. In general the system is less unstable when the CR diffusion coefficient is smaller (i.e., the coupling between the CRs and plasma is stronger). The system is also less unstable if CR pressure is larger. This is a reminiscence of the fact that Jeans instability and Parker instability are less unstable when the gas pressure is larger (or temperature is higher). Moreover, for large CR diffusion coefficient (or small CR pressure), perturbations parallel to the magnetic field are more unstable than those perpendicular to it. The other governing factor on the growth rate of the perturbations in different directions is the thickness of the disk or the strength of the external pressure on the disk. In fact, this is the determining factor in some parameter regimes.

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