MAGNETOROTATIONAL CORE-COLLAPSE SUPERNOVAE IN THREE DIMENSIONS

被引：204

作者：

Moesta, Philipp ^{[1
]}

Richers, Sherwood ^{[1
]}

Ott, Christian D. ^{[1
,2
]}

Haas, Roland ^{[1
]}

Piro, Anthony L. ^{[1
]}

Boydstun, Kristen ^{[1
]}

Abdikamalov, Ernazar ^{[1
]}

Reisswig, Christian ^{[1
]}

Schnetter, Erik ^{[3
,4
,5
]}

机构：

[1] CALTECH, TAPIR, Pasadena, CA 91125 USA

[2] Univ Tokyo, Kavli IPMU WPI, Kashiwa, Chiba, Japan

[3] Perimeter Inst Theoret Phys, Waterloo, ON, Canada

[4] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada

[5] Louisiana State Univ, Ctr Computat & Technol, Baton Rouge, LA 70803 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2014年 / 785卷 / 02期

基金：

美国国家科学基金会;

关键词：

gamma-ray burst: general; instabilities; magnetohydrodynamics (MHD); neutrinos supernovae:general; 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; GAMMA-RAY BURSTS; INSTABILITY; MODEL; STARS; DISKS; JETS;

D O I：

10.1088/2041-8205/785/2/L29

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present results of new three-dimensional (3D) general-relativistic magnetohydrodynamic simulations of rapidly rotating strongly magnetized core collapse. These simulations are the first of their kind and include a microphysical finite-temperature equation of state and a leakage scheme that captures the overall energetics and lepton number exchange due to postbounce neutrino emission. Our results show that the 3D dynamics of magnetorotational core collapse supernovae are fundamentally different from what was anticipated on the basis of previous simulations in axisymmetry (2D). A strong bipolar jet that develops in a simulation constrained to 2D is crippled by a spiral instability and fizzles in full 3D. While multiple (magneto-) hydrodynamic instabilities may be present, our analysis suggests that the jet is disrupted by an m = 1 kink instability of the ultra-strong toroidal field near the rotation axis. Instead of an axially symmetric jet, a completely new, previously unreported flow structure develops. Highly magnetized spiral plasma funnels expelled from the core push out the shock in polar regions, creating wide secularly expanding lobes. We observe no runaway explosion by the end of the full 3D simulation 185 ms after bounce. At this time, the lobes have reached maximum radii of similar to 900 km.

引用

页数：6