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Axisymmetric simulations of magneto--rotational core collapse: dynamics and gravitational wave signal | | M. Obergaulinger
; M.A. Aloy
; E. Mueller
; | | Date: |
6 Oct 2005 | | Subject: | astro-ph | | Abstract: | We have performed a comprehensive parameter study of the collapse of rotating, strongly magnetized stellar cores in axisymmetry to determine their gravitational wave signature based on the Einstein quadrupole formula. We use a Newtonian explicit magnetohydrodynamic Eulerian code based on the relaxing-TVD method for the solution of the ideal MHD equations, and apply the constraint-transport method to guarantee a divergence--free evolution of the magnetic field. We neglect effects due to neutrino transport and employ a simplified equation of state. The pre--collapse initial models are polytropes in rotational equilibrium with a prescribed degree of differential rotation and rotational energy (~ 1 % of the gravitational energy). The initial magnetic fields are purely poloidal the field strength ranging from 10^10 G to 10^13 G. The evolution of the core, whose collapse is initiated by reducing the gas pressure by a prescribed amount, is followed until a few ten milliseconds past core bounce. The initial magnetic fields are amplified mainly by the differential rotation of the core giving rise to a strong toroidal field component. The poloidal field component grows by compression during collapse, but does not change significantly after core bounce if (abbreviated) | | Source: | arXiv, astro-ph/0510184 | | Services: | Forum | Review | PDF | Favorites | |
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