TURBULENT MAGNETIC FIELD AMPLIFICATION FROM SPIRAL SASI MODES: IMPLICATIONS FOR CORE-COLLAPSE SUPERNOVAE AND PROTO-NEUTRON STAR MAGNETIZATION

被引：76

作者：

Endeve, Eirik ^{[1
]}

Cardall, Christian Y. ^{[2
,3
]}

Budiardja, Reuben D. ^{[2
,3
,4
,5
]}

Beck, Samuel W. ^{[4
]}

Bejnood, Alborz ^{[4
]}

Toedte, Ross J. ^{[6
]}

Mezzacappa, Anthony ^{[1
,2
,3
]}

Blondin, John M. ^{[7
]}

机构：

[1] Oak Ridge Natl Lab, Comp Sci & Math Div, Oak Ridge, TN 37831 USA

[2] Oak Ridge Natl Lab, Div Phys, Oak Ridge, TN 37831 USA

[3] Univ Tennessee, Dept Phys & Astron, Knoxville, TN 37996 USA

[4] Oak Ridge Natl Lab, Joint Inst Heavy Ion Res, Oak Ridge, TN 37831 USA

[5] Univ Tennessee, Natl Inst Computat Sci, Knoxville, TN 37996 USA

[6] Oak Ridge Natl Lab, Natl Ctr Computat Sci, Oak Ridge, TN 37831 USA

[7] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA

来源：

ASTROPHYSICAL JOURNAL | 2012年 / 751卷 / 01期

关键词：

magnetohydrodynamics (MHD); methods: numerical; stars: magnetic field; supernovae: general turbulence; NONHELICAL HYDROMAGNETIC TURBULENCE; GODUNOV-TYPE SCHEMES; ACCRETION-SHOCK; DRIVEN SUPERNOVA; RIEMANN SOLVER; DYNAMO ACTION; SIMULATIONS; INSTABILITY; TRANSPORT; GENERATION;

D O I：

10.1088/0004-637X/751/1/26

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We extend our investigation of magnetic field evolution in three-dimensional flows driven by the stationary accretion shock instability (SASI) with a suite of higher-resolution idealized models of the post-bounce core-collapse supernova environment. Our magnetohydrodynamic simulations vary in initial magnetic field strength, rotation rate, and grid resolution. Vigorous SASI-driven turbulence inside the shock amplifies magnetic fields exponentially; but while the amplified fields reduce the kinetic energy of small-scale flows, they do not seem to affect the global shock dynamics. The growth rate and final magnitude of the magnetic energy are very sensitive to grid resolution, and both are underestimated by the simulations. Nevertheless, our simulations suggest that neutron star magnetic fields exceeding 10(14) G can result from dynamics driven by the SASI, even for non-rotating progenitors.

引用

页数：28

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