Open AccessA magnetorotational core‐collapse model with jets
Author(s) -
Moiseenko S. G.,
BisnovatyiKogan G. S.,
Ardeljan N. V.
Publication year - 2006
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2006.10517.x
Subject(s) - physics , magnetorotational instability , magnetic field , astrophysics , quadrupole , core (optical fiber) , gravitational collapse , dipole , jet (fluid) , magnetic dipole , magnetohydrodynamics , mechanics , atomic physics , optics , quantum mechanics
We present the results of the 2D simulation of a magnetorotational (MR) core‐collapse model accompanied by jet formation in the core‐collapse model explosion. The initial magnetic field used in the simulations has a dipole‐like symmetry. Contrary to the simulations of the MR core‐collapse model with an initial quadrupole‐like magnetic field, where the matter was ejected mainly near the equatorial plane, in the presence of the dipole‐like initial magnetic field the core‐collapse model explosion is developing preferably along a rotational axis and leads to the formation of a protojet. We expect that protojet propagation through the envelope of the star will be accompanied by its collimation. The magnetorotational instability (MRI) was found in the simulations, similar to the earlier considered case of the quadrupole‐like initial magnetic field. Our estimations show that the characteristic time for the reconnection of the magnetic field is much larger than the MRI development time. The supernova explosion energy for the dipole‐like field is about 0.61 × 10 51 erg , and about 0.13 M ⊙ of mass was ejected during the explosion.