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Magnetorotational Core-collapse Supernovae in Three Dimensions

Mösta, Philipp and Richers, Sherwood and Ott, Christian D. and Haas, Roland and Piro, Anthony L. and Boydstun, Kristen and Abdikamalov, Ernazar and Reisswig, Christian and Schnetter, Erik (2014) Magnetorotational Core-collapse Supernovae in Three Dimensions. Astrophysical Journal Letters, 785 (2). L29. ISSN 2041-8205.

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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 ~900 km.

Item Type:Article
Related URLs:
URLURL TypeDescription and further details on simulations Paper
Mösta, Philipp0000-0002-9371-1447
Richers, Sherwood0000-0001-5031-6829
Ott, Christian D.0000-0003-4993-2055
Haas, Roland0000-0003-1424-6178
Piro, Anthony L.0000-0001-6806-0673
Schnetter, Erik0000-0002-4518-9017
Additional Information:© 2014. The American Astronomical Society. Received 6 March 2014, accepted for publication 24 March 2014. Published 3 April 2014. The authors would like to thank A. Burrows, S. Couch, U. Gamma, D. Meier, and L. Roberts for discussions. This research was partially supported by NSF grants AST-1212170, PHY-1151197, and OCI-0905046, and the Sherman Fairchild Foundation. S.R. is supported by a DOE Computational Science Graduate Fellowship DE-FG02-97ER25308. C.R. acknowledges support by NASA through Einstein Fellowship grant PF2-130099. The simulations were carried out on XSEDE (TG-PHY100033) and on NSF/NCSA BlueWaters (PRAC OCI-0941653).
Funding AgencyGrant Number
Sherman Fairchild FoundationUNSPECIFIED
Department of Energy (DOE)DE-FG02-97ER25308
NASA Einstein FellowshipPF2-130099
Subject Keywords:gamma-ray burst: general – instabilities – magnetohydrodynamics (MHD) – neutrinos – supernovae: general
Issue or Number:2
Record Number:CaltechAUTHORS:20140424-194106351
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:45202
Deposited By: George Porter
Deposited On:25 Apr 2014 03:48
Last Modified:09 Mar 2020 13:19

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