[14.06] Feedback Effects of the Magnetorotational Instability on Core Collapse Supernovae

AAS 200th meeting, Albuquerque, NM, June 2002
Session 14. Supernovae
Display, Monday, June 3, 2002, 9:20am-6:30pm, SW Exhibit Hall

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[14.06] Feedback Effects of the Magnetorotational Instability on Core Collapse Supernovae

S. Akiyama, J. C. Wheeler (University of Texas at Austin), D. L. Meier (Jet Propulsion Laboratory), I. Lichtenstadt (Hebrew University)

We continue our investigation of the effects of the magnetorotational instability (MRI) on collapsing, rotating iron cores. A weak seed field will be exponentially amplified with a growth time t~1/\Omega to produce a magnetic field with strength 10¹⁴-10¹⁶ G within 300 msec after bounce. We follow the collapse with a one-dimensional flux-limited diffusion numerical code. In new work, we explore cylindrical symmetry for angular velocity profiles and invoke a centrifugal quasi-potential to allow somewhat higher initial angular rotation to be explored. We investigate the effect of convection in the core collapse environment to enhance or inhibit the growth of magnetic field, and also explore the feedback effects of the magnetic pressure and viscous drag. The rapid growth of the magnetic field may promote the formation of MHD jets up the rotation axis and, ultimately, a supernova explosion. This research is supported by NASA Grant NAG5-10766 and NSF Grant AST-0098644.

The author(s) of this abstract have provided an email address for comments about the abstract: shizuka@astro.as.utexas.edu

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