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A large scale dynamo and magnetoturbulence in rapidly rotating core-collapse supernovae

Mösta, Philipp and Ott, Christian D. and Radice, David and Roberts, Luke F. and Schnetter, Erik and Haas, Roland (2015) A large scale dynamo and magnetoturbulence in rapidly rotating core-collapse supernovae. Nature, 528 (7582). pp. 376-379. ISSN 0028-0836. http://resolver.caltech.edu/CaltechAUTHORS:20150914-145343070

[img] Image (JPEG) (Extended Data Figure 1: Evolution of the maximum poloidal magnetic field) - Supplemental Material
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[img] Image (JPEG) (Extended Data Figure 2: Background flow stability analysis) - Supplemental Material
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[img] Image (JPEG) (Extended Data Figure 3: Angle-averaged poloidal magnetic current and magnetic flux) - Supplemental Material
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[img] Image (JPEG) (Extended Data Figure 4: Angle-averaged poloidal magnetic current and velocity vectors) - Supplemental Material
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[img] Image (JPEG) (Extended Data Figure 5: AMR stellar collapse simulation) - Supplemental Material
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[img] Image (JPEG) (Extended Data Figure 6: AMR stellar collapse simulation) - Supplemental Material
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[img] Image (JPEG) (Extended Data Figure 7: Non-densitized turbulent kinetic and electromagnetic energy spectra) - Supplemental Material
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Abstract

Magnetohydrodynamic turbulence is important in many high-energy astrophysical systems, where instabilities can amplify the local magnetic field over very short timescales. Specifically, the magnetorotational instability and dynamo action have been suggested as a mechanism for the growth of magnetar-strength magnetic fields (of 10^(15) gauss and above) and for powering the explosion of a rotating massive star. Such stars are candidate progenitors of type Ic-bl hypernovae, which make up all supernovae that are connected to long γ-ray bursts. The magnetorotational instability has been studied with local high-resolution shearing-box simulations in three dimensions, and with global two-dimensional simulations, but it is not known whether turbulence driven by this instability can result in the creation of a large-scale, ordered and dynamically relevant field. Here we report results from global, three-dimensional, general-relativistic magnetohydrodynamic turbulence simulations. We show that hydromagnetic turbulence in rapidly rotating protoneutron stars produces an inverse cascade of energy. We find a large-scale, ordered toroidal field that is consistent with the formation of bipolar magnetorotationally driven outflows. Our results demonstrate that rapidly rotating massive stars are plausible progenitors for both type Ic-bl supernovae and long γ-ray bursts, and provide a viable mechanism for the formation of magnetars. Moreover, our findings suggest that rapidly rotating massive stars might lie behind potentially magnetar-powered superluminous supernovae.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1038/nature15755DOIArticle
http://www.nature.com/nature/journal/vaop/ncurrent/full/nature15755.htmlPublisherArticle
http://rdcu.be/e6mpPublisherFree ReadCube access
ORCID:
AuthorORCID
Ott, Christian D.0000-0003-4993-2055
Roberts, Luke F.0000-0001-7364-7946
Additional Information:© 2015 Macmillan Publishers Limited. Received 7 April; accepted 23 September 2015. Published online 30 November 2015. We thank S. Couch, J. Zrake, D. Tsang, C. Wheeler, E. Bentivegna and I. Hinder for discussions. This research was supported by National Science Foundation (NSF) grants AST-1212170, PHY-1151197 and OCI-0905046; by NASA through the Einstein Fellowship Program, grants PF5-160140 (to P.M.) and PF3-140114 (to L.F.R.); by a National Science and Engineering Research Council of Canada (NSERC) award to E.S.; and by the Sherman Fairchild Foundation. The simulations were carried out on the NSF/National Center for Supercomputing Applications (NCSA) BlueWaters supercomputer (PRAC ACI-1440083). Author Contributions: P.M. contributed to project planning and leadership, simulation code development, simulations, simulation analysis, visualization, interpretation of results and manuscript preparation. C.D.O. led the group, conceived the idea for the project, and contributed to project planning and leadership, interpretation and manuscript preparation. D.R. contributed to simulation analysis, interpretation, simulation code development and manuscript preparation. L.F.R. interpreted the results and reviewed the manuscript. E.S. contributed to simulation code development and manuscript review. R.H. contributed to development of the simulation code and visualization software, and reviewed the manuscript. The authors declare no competing financial interests.
Group:TAPIR, Walter Burke Institute for Theoretical Physics
Funders:
Funding AgencyGrant Number
NSFAST-1212170
NSFPHY-1151197
NSFOCI-0905046
NASA Einstein Postdoctoral FellowshipPF5-160140
NASA Einstein Postdoctoral FellowshipPF3-140114
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Sherman Fairchild FoundationUNSPECIFIED
NSFACI-1440083
Record Number:CaltechAUTHORS:20150914-145343070
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20150914-145343070
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:60231
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:29 Nov 2015 20:46
Last Modified:10 Apr 2017 18:38

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