Magnetorotational supernovae. Magnetorotational instability. Jet formation |
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Authors: | Sergey G Moiseenko Gennady S Bisnovatyi-Kogan |
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Institution: | (1) Space Research Institute, Profsoyuznaya str. 84/32, Moscow, 117997, Russia |
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Abstract: | 2D numerical simulations of magnetorotational (MR) supernova mechanism are described. It is shown that magnetic field is amplified
due to the differential rotation after core collapse. When magnetic pressure reaches some level, a compression wave starts
to move outwards. Moving along steeply decreasing density profile the compression wave transforms quickly into fast MHD shock.
The magnetorotational instability (MRI) was found in our simulations. MRI leads to the exponential growth of the components
of the magnetic field. The MRI significantly reduces MR supernova explosion time. Configuration of the initial magnetic field
qualitatively defines the shape of MR supernova explosion. For the quadrupole-like initial poloidal field the MR supernova
explosion develops mainly along equatorial plane, the dipole-like initial field results in MR supernova developing as mildly
collimated jet along axis of rotation. The explosion energy of MR supernova found in our simulations is ∼0.5–0.6×1051 erg. |
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Keywords: | (Stars:) supernovae: general |
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