Turbulence and magnetic field amplification from spiral SASI modes in core-collapse supernovae

E. Endeve, C. Y. Cardall, R. D. Budiardja, A. Mezzacappa, J. M. Blondin

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9 Scopus citations

Abstract

The stationary accretion shock instability (SASI) plays a central role in modern simulations of the explosion phase of core-collapse supernovae (CCSNe). It may be key to realizing neutrino powered explosions, and possibly links birth properties of pulsars (e.g., kick, spin and magnetic field) to supernova dynamics. Using high-resolution magnetohydrodynamic simulations, we study the development of turbulence, and subsequent amplification of magnetic fields in a simplified model of the post-bounce CCSN environment. Turbulence develops from secondary instabilities induced by the SASI. Our simulations suggest that the development of turbulence plays an important role for the subsequent evolution of the SASI. The turbulence also acts to amplify weak magnetic fields via a small-scale dynamo.

Original languageEnglish
Article number014022
JournalPhysica Scripta
Volume88
Issue numberT155
DOIs
StatePublished - Jul 2013

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