Fluid Instabilities of Magnetar-Powered Supernovae
arXiv:1706.06761 · doi:10.1088/1742-6596/837/1/012006
Abstract
Magnetar-powered supernova explosions are competitive models for explaining very luminous optical transits. However, these explosion models were mainly calculated in 1D. Radiation emitted from the magnetar snowplows into the previous supernovae ejecta and causes a nonphysical dense shell (spike) found in previous 1D studies. This suggests that strong fluid instabilities may have developed within the magnetar-powered supernovae. Such fluid instabilities emerge at the region where luminous transits later occur, so they can affect the consequent observational signatures. We examine the magnetar-powered supernovae with 2D hydrodynamics simulations and find that the 1D dense shell transforms into the development of Rayleigh-Taylor and thin shell instabilities in 2D. The resulting mixing is able to fragment the entire shell and break the spherical symmetry of supernovae ejecta.
Proceedings of 11th International Conference on Numerical Modeling of Space Plasma Flows: ASTRONUM-2016
References in corpus (5)
- The Supernova -- Gamma-Ray Burst Connection
- The strongest cosmic magnets: Soft Gamma-ray Repeaters and Anomalous X-ray Pulsars
- The Unique Type Ib Supernova 2005bf at Nebular Phases: A Possible Birth Event of A Strongly Magnetized Neutron Star
- Criteria for Core-Collapse Supernova Explosions by the Neutrino Mechanism
- Spin-down rate and inferred dipole magnetic field of the soft gamma-ray repeater SGR 1627-41