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Local Simulations of the Magneto-rotational Instability in Core-Collapse Supernovae by Masada, Y.; Takiwaki, T.; Kotake, K.; Sano, T. is a scholarly article available to read on EtoBox.

What is Local Simulations of the Magneto-rotational Instability in Core-Collapse Supernovae about?

Bearing in mind the application to core-collapse supernovae, we study nonlinear properties of the magneto-rotational instability (MRI) by means of three- dimensional simulations in the framework of a local shearing box approximation. By changing systematically the shear rates that symbolize the degree of differential rotation in nascent proto-neutron stars (PNSs), we derive a scaling relation between the turbulent stress sustained by the MRI and the shear- vorticity ratio. Our parametric survey shows a power-law scaling between the turbulent stress ($<< w_{\rm tot}>>$) and the shear- vorticity ratio ($g_q$) as $<<w_{\rm tot}>> \propto g_q^{\delta}$ with its index $\delta \sim 0.5$. The MRI-amplified magnetic energy has a similar scaling relative to the turbulent stress, while the Maxwell stress has slightly smaller power-law index ($\sim 0.36$). By modeling the effect of viscous heating rates due to the MRI turbulence, we show that the stronger magnetic fields or the larger shear rates initially imposed lead to the higher dissipation rates. For a rapidly rotating PNS with the spin period in milliseconds and with strong magnetic fields of $10^{15}$ G, the energy dissipation rate is

Author

Masada, Y.; Takiwaki, T.; Kotake, K.; Sano, T.

Published

2012

Language

EN