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

Conference · Tue Jan 01 04:00:00 EST 2013

OSTI ID:1088109

Endeve, Eirik ^[1]; Cardall, Christian Y ^[1]; Budiardja, Reuben D ^[1]; Blondin, John ^[1]; Mezzacappa, Anthony ^[1]

---

1. ORNL

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 core-collapse supernova 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.

• Research Organization: Oak Ridge National Laboratory (ORNL); Center for Computational Sciences
• Sponsoring Organization: USDOE
• DOE Contract Number: AC05-00OR22725
• OSTI ID: 1088109
• Country of Publication: United States
• Language: English