Global Simulations of the Magnetorotational Instability in a Spherical Geometry

Details Global Simulations of the Magnetorotational Instability in a Spherical Geometry Global Simulations of the Magnetorotational Instability in a Spherical Geometry

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.8903k&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #89.03; Bulletin of the American Astronomical Society, V

Astronomy and Astrophysics

Astronomy

Scientific paper

We explore the action of the magnetorotational instability (MRI) in a spherical geometry. Though often discussed in relation to accretion disks, the MRI, which occurs in the presence of a weak magnetic field in a differentially rotating plasma, is relevant to numerous phenomena in magnetized rotating stars. Here we use global MHD simulations to examine the non-linear development of this instability in differentially rotating polytropes. We conduct our simulations with an Eulerian grid code that includes self-gravity. Our results are most applicable to the radiative zones of solar-type stars; implications for degenerate stars are also discussed.

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