The Three Dimensional MHD Effects For Core Collapse Supernova Explosion
We show three-dimensional numerical simulations on the core collapse of a rotating massive star threaded by strong magnetic fields. The initial magnetic field is nearly uniform in the core and inclined with respect to the rotation axis. We have made 17 models having different angular velocity and magnetic field of the progenitor. All the models show nearly spherical prompt shock just after the core bounce. The magnetic field is amplified by rotation in a torus region around the protoneutron star. The azimuthal component of magnetic field changes its sign with a semi-regular interval in the torus. This is due to the inclination of initial magnetic field. After the twisted magnetic field is accumulated, the bipolar jets are launched along the initial rotation axis. When the initial magnetic field is weak, the magnetic energy is dissipated substantially by numerical diffusion before the launch of jets.
Accretion accretion disks-methods numerical-MHD-supernovae general
Hayato Mikami Yuji Sato Tomoaki Matsumoto Tomoyuki Hanawa
Graduate School of Science, Chiba University 1-33, Yayoi-cho, Inage-ku, Chiba 263-8522, Japan Faculty of Humanity and Environment, Hosei University, Fujimi, Chiyoda-ku, Tokyo 102-8160 Japan Center for Frontier Science, Chiba University, 1-33, Yayoi-cho, Inage-ku, Chiba 263-8522, Japan
国际会议
紧凑型物体的天体物理学国际会议(International Conference on Astrophysics of Compact Objects)
安徽黄山
英文
49-52
2007-07-01（万方平台首次上网日期，不代表论文的发表时间）