Display options
Cite
Mösta P, Ott CD, Radice D, et al. A large-scale dynamo and magnetoturbulence in rapidly rotating core-collapse supernovae. Nature. 2015;528(7582):376-9doi: 10.1038/nature15755.
Mösta, P., Ott, C. D., Radice, D., Roberts, L. F., Schnetter, E., & Haas, R. (2015). A large-scale dynamo and magnetoturbulence in rapidly rotating core-collapse supernovae. Nature, 528(7582), 376-9. https://doi.org/10.1038/nature15755
Mösta, Philipp, et al. "A large-scale dynamo and magnetoturbulence in rapidly rotating core-collapse supernovae." Nature vol. 528,7582 (2015): 376-9. doi: https://doi.org/10.1038/nature15755
Mösta P, Ott CD, Radice D, Roberts LF, Schnetter E, Haas R. A large-scale dynamo and magnetoturbulence in rapidly rotating core-collapse supernovae. Nature. 2015 Dec 17;528(7582):376-9. doi: 10.1038/nature15755. Epub 2015 Nov 30. PMID: 26618868.
Copy Download .nbib Format: NLM
Share it on

Nature. 2015 Dec 17;528(7582):376-9. doi: 10.1038/nature15755. Epub 2015 Nov 30.

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

Nature

Philipp Mösta, Christian D Ott, David Radice, Luke F Roberts, Erik Schnetter, Roland Haas

Affiliations

  1. TAPIR, Walter Burke Institute for Theoretical Physics, Mailcode 350-17, California Institute of Technology, Pasadena, California 91125, USA.
  2. Department of Astronomy, 501 Campbell Hall #3411, University of California at Berkeley, Berkeley, California 94720, USA.
  3. Perimeter Institute for Theoretical Physics, Waterloo, Ontario N2L 2Y5, Canada.
  4. Department of Physics, University of Guelph, Guelph, Ontario N1G 2W1, Canada.
  5. Center for Computation &Technology, Louisiana State University, Baton Rouge, Louisiana, 70803, USA.
  6. Max Planck Institute for Gravitational Physics, Am Mühlenberg 1, 14476 Potsdam-Golm, Germany.

PMID: 26618868 DOI: 10.1038/nature15755

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.

References

  1. Nature. 2006 Aug 31;442(7106):1014-7 - PubMed
  2. Nature. 2013 Oct 17;502(7471):346-9 - PubMed
  3. Nature. 2015 Jul 9;523(7559):189-92 - PubMed

Publication Types