Magnetic field generation by the stationary accretion shock instability

Abstract

By adding a weak magnetic field to a spherically symmetric fluid configuration that caricatures a stalled shock in the post-bounce supernova environment, we explore the capacity of the stationary accretion shock instability (SASI) to generate magnetic fields. The SASI develops upon perturbation of the initial condition, and the ensuing flow generates--{\em in the absence of rotation}--dynamically significant magnetic fields ($\sim 10^{15}$ G) on a time scale that is relevant for the explosion mechanism of core-collapse supernovae. We describe our model, present some recent results, and discuss their potential relevance for supernova models.

5 pages, 3 figures, submitted to Journal of Physics: Conference Series, SciDAC 2008

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Cited by in corpus (3)

• Magnetic field amplification and magnetically supported explosions of collapsing, non-rotating stellar cores
• Effects of Rotation on Standing Accretion Shock Instability in Nonlinear Phase for Core-Collapse Supernovae
• Direct time radio variability induced by non-axisymmetric standing accretion shock instability: implications for M87