Help Privacy Policy Disclaimer
  Advanced SearchBrowse




Journal Article

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


Mösta,  Philipp
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

External Resource
No external resources are shared
Fulltext (public)

(Preprint), 9MB

Supplementary Material (public)
There is no public supplementary material available

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), 376-379. doi:10.1038/nature15755.

Cite as: http://hdl.handle.net/11858/00-001M-0000-0029-5B2C-2
Magnetohydrodynamic (MHD) turbulence is of key importance in many high-energy astrophysical systems, including black-hole accretion disks, protoplanetary disks, neutron stars, and stellar interiors. MHD instabilities can amplify local magnetic field strength over very short time scales, but it is an open question whether this can result in the creation of a large scale ordered and dynamically relevant field. Specifically, the magnetorotational instability (MRI) has been suggested as a mechanism to grow magnetar-strength magnetic field ($\gtrsim 10^{15}\, \mathrm{G}$) and magnetorotationally power the explosion of a rotating massive star. Such stars are progenitor candidates for type Ic-bl hypernova explosions that involve relativistic outflows and make up all supernovae connected to long gamma-ray bursts (GRBs). We have carried out global 3D general-relativistic magnetohydrodynamic (GRMHD) turbulence simulations that resolve the fastest growing mode (FGM) of the MRI. We show that MRI-driven MHD turbulence in rapidly rotating protoneutron stars produces a highly efficient inverse cascade of magnetic energy. This builds up magnetic energy on large scales whose magnitude rivals the turbulent kinetic energy. We find a large-scale ordered toroidal field along the rotation axis of the protoneutron star 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 GRBs, present a viable formation scenario for magnetars, and may account for potentially magnetar-powered superluminous supernovae.