Numerical Study on the Rotational Collapse of Strongly Magnetized Cores of Massive Stars

Details Numerical Study on the Rotational Collapse of Strongly Magnetized Cores of Massive Stars Numerical Study on the Rotational Collapse of Strongly Magnetized Cores of Massive Stars

Jun 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004apj...608..907y&link_type=abstract

The Astrophysical Journal, Volume 608, Issue 2, pp. 907-924.

Astronomy and Astrophysics

Astronomy

56

Magnetohydrodynamics: Mhd, Stars: Pulsars: General, Stars: Evolution, Stars: Magnetic Fields, Stars: Supernovae: General-

Scientific paper

Hydrodynamics of the rotational collapse of strongly magnetized massive stellar cores has been studied numerically. Employing simplified microphysics and a two-dimensional nonrelativistic MHD code, we have performed a parametric research with respect to the strength of magnetic field and rotation, paying particular attention to the systematics of dynamics. We assume initially that the rotation is almost uniform and the magnetic field is constant in space and parallel to the rotation axis. The initial angular velocity and magnetic field strength span 1.7-6.8 rad s-1 and (1.8-5.8)×1012 G, respectively. We have found that the combination of rotation and magnetic field can lead to a jetlike prompt explosion in the direction of the rotational axis, which would not be produced by either of them alone. The range of the maximum angular velocity and field strength is 2.3×10-3to5.8×10-4 rad s-1 and 2.3×1015to5.6×1016 G, respectively, at the end of computations. Although the results appear to be consistent with those by LeBlanc & Wilson and Symbalisty, the magnetic fields behind the shock wave, not in the inner core, are the main driving factor of the jet in our models. The fields are amplified by the strong differential rotations in the region between the shock wave and the boundary of the inner and outer cores, enhanced further by the lateral matter motions induced either by an oblique shock wave (for a strong shock case) or possibly by the MRI (magnetorotational instability)-like instability (for a weak shock case). We have also calculated the gravitational wave forms in the quadrupole approximation. Although the wave form from a nonrotating magnetic core is qualitatively different from those from rotating cores, the amplitude is about an order of magnitude smaller. Otherwise, we have found no substantial difference in the first burst of gravitational waves among the magnetized and nonmagnetized models, since the bounce is mainly driven by the combination of the matter pressure and the centrifugal force.

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