A 3D simulation of a neutrino-driven supernova explosion aided by convection and magnetic fields. (14th August 2020)

• Record Type: Journal Article
• Authors: Müller, Bernhard; Varma, Vishnu
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 498:Number 1(2020)
• Page Start: L109
• Page End: L113
• Publication Date: 2020-08-14
• Subjects: MHD -- turbulence -- supernovae: general; Astronomy -- Research -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnrasl/slaa137
• Languages: English
• ISSNs: 1745-3933

Abstract

ABSTRACT: We study the impact of a small-scale dynamo in core-collapse supernovae using a 3D neutrino magnetohydrodynamics (MHD) simulation of a 15 M⊙ progenitor. The weak seed field is amplified exponentially in the gain region once neutrino-driven convection develops, and remains dominated by small-scale structures. About $250\, \mathrm{ms}$ after bounce, the field energy in the gain region reaches ${\sim } 50{{\ \rm per\ cent}}$ of kinetic equipartition. This supports the development of a neutrino-driven explosion with modest global anisotropy, which does not occur in a corresponding model without magnetic fields. Our results suggest that magnetic fields may play a beneficial subsidiary role in neutrino-driven supernovae even without rapid progenitor rotation. Further investigation into the nature of MHD turbulence in the supernova core is required.