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Title: Generation of Magnetic Fields by the Stationary Accretion Shock Instability

Journal Article · · Astrophysical Journal
 [1];  [1];  [2];  [1]
  1. ORNL
  2. University of Tennessee, Knoxville (UTK)
+ Show Author Affiliations

We begin an exploration of the capacity of the stationary accretion shock instability (SASI) to generate magnetic fields by adding a weak, stationary, and radial (but bipolar) magnetic field, and in some cases rotation, to an initially spherically symmetric fluid configuration that models a stalled shock in the post-bounce supernova environment. In axisymmetric simulations we find that cycles of latitudinal flows into and radial flows out of the polar regions amplify the field parallel to the symmetry axis, typically increasing the total magnetic energy by about two orders of magnitude. Nonaxisymmetric calculations result in fundamentally different flows and a larger magnetic energy increase: shearing associated with the SASI spiral mode contributes to a widespread and turbulent field amplification mechanism, boosting the magnetic energy by almost four orders of magnitude (a result which remains very sensitive to the spatial resolution of the numerical simulations). While the SASI may contribute to neutron star magnetization, these simulations do not show qualitatively new features in the global evolution of the shock as a result of SASI-induced magnetic field amplification.

Research Organization:
Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Oak Ridge Leadership Computing Facility (OLCF); Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). National Center for Computational Sciences (NCCS)
Sponsoring Organization:
USDOE Office of Science (SC)
DOE Contract Number:
DE-AC05-00OR22725
OSTI ID:
985751
Journal Information:
Astrophysical Journal, Vol. 713, Issue 2; ISSN 0004-637X
Country of Publication:
United States
Language:
English

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71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
AMPLIFICATION
CAPACITY
CONFIGURATION
EXPLORATION
INSTABILITY
MAGNETIC FIELDS
MAGNETIZATION
NEUTRON STARS
POLAR REGIONS
ROTATION
SPATIAL RESOLUTION
SYMMETRY