Magnetohydrodynamic Rebound Shocks of Supernovae

Details Magnetohydrodynamic Rebound Shocks of Supernovae Magnetohydrodynamic Rebound Shocks of Supernovae

2007-04-02

arxiv.org/abs/0704.0223v1

Mon.Not.Roy.Astron.Soc.Lett.378:L54-L58,2007

Astronomy and Astrophysics

Astrophysics

5 pages, 1 figure, Accepted for publication in MNRAS

Scientific paper

10.1111/j.1745-3933.2007.00319.x

We construct magnetohydrodynamic (MHD) similarity rebound shocks joining `quasi-static' asymptotic solutions around the central degenerate core to explore an MHD model for the evolution of random magnetic field in supernova explosions. This provides a theoretical basis for further studying synchrotron diagnostics, MHD shock acceleration of cosmic rays, and the nature of intense magnetic field in compact objects. The magnetic field strength in space approaches a limiting ratio, that is comparable to the ratio of the ejecta mass driven out versus the progenitor mass, during this self-similar rebound MHD shock evolution. The intense magnetic field of the remnant compact star as compared to that of the progenitor star is mainly attributed to both the gravitational core collapse and the radial distribution of magnetic field.

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