MHD Simulations of Core Collapse Supernovae with Cosmos++

Details MHD Simulations of Core Collapse Supernovae with Cosmos++ MHD Simulations of Core Collapse Supernovae with Cosmos++

2010-08-08

arxiv.org/abs/1008.1422v1

Astronomy and Astrophysics

Astrophysics

High Energy Astrophysical Phenomena

3 pages, 2 figures. To appear in the proceedings of the "Deciphering the Ancient Universe with Gamma-Ray Bursts", April 2010,

Scientific paper

We performed 2D, axisymmetric, MHD simulations with Cosmos++ in order to examine the growth of the magnetorotational instability (MRI) in core--collapse supernovae. We have initialized a non--rotating 15 solar mass progenitor, infused with differential rotation and poloidal magnetic fields. The collapse of the iron core is simulated with the Shen EOS, and the parametric Ye and entropy evolution. The wavelength of the unstable mode in the post--collapse environment is expected to be only ~ 200 m. In order to achieve the fine spatial resolution requirement, we employed remapping technique after the iron core has collapsed and bounced. The MRI unstable region appears near the equator and angular momentum and entropy are transported outward. Higher resolution remap run display more vigorous overturns and stronger transport of angular momentum and entropy. Our results are in agreement with the earlier work by Akiyama et al. (2003) and Obergaulinger et al. (2009).

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