The stability of protostellar disks with Hall effect and buoyancy

Details The stability of protostellar disks with Hall effect and buoyancy The stability of protostellar disks with Hall effect and buoyancy

2003-07-10

arxiv.org/abs/astro-ph/0307198v1

Astronomy and Astrophysics

Astrophysics

8 pages, 2 figures, submitted to Astron. Astrophys

Scientific paper

The stability properties of inviscid protostellar disks are examined taking into account the Hall effect and buoyancy. Depending on the parameters, different types of instabilities can exist in different regions of disks. In a very low ionized region, the instability associated with baroclinic effects of buoyancy is likely most efficient. The Hall-driven shear instability can lead to destabilization of regions with a higher ionization. The magnetorotational instability modified by buoyancy can only be a destabilizing factor in regions with strong magnetic field or a relatively high conductivity ($\sigma B^2 / \rho > a_e \Omega$, with $a_e$ the magnetization parameter of electrons).

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