Fluid Instabilities of Magnetar-Powered Supernovae

11th International Conference on Numerical Modeling of Space Plasma Flows

Chen, Ke-Jung^1

Division of Theoretical Astronomy, National Astronomical Observatory of Japan, Tokyo

181-8588, Japan^1

关键词: Competitive models;    Dense shells;    Explosion models;    Fluid instability;    Hydrodynamics simulations;    Rayleigh-Taylor;    Spherical symmetry;    Supernova explosion;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/837/1/012006/pdf
DOI  :  10.1088/1742-6596/837/1/012006

来源: IOP

【 摘 要 】

Magnetar-powered supernova explosions are competitive models for explaining very luminous optical transits. Until recently, 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.