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Paper: An Approximate Riemann Solver for the MHD Equations and Its Application to type II Supernova
Volume: 359, Numerical Modeling of Space Plasma Flows: Astronum-2006
Page: 158
Authors: Hanawa, T.; Mikami, H.; Sato, Y.; Matsumoto, T.
Abstract: We show 3D MHD simulations in which a massive star collapses to form a proto-neutron star having magnetic field inclined to its rotation axis. The simulations take account of equation of state of high density gas as well as self-gravity and magnetic field. We solved the MHD equations with a Roe-type approximate Riemann solver. High spatial resolution and wide dynamic range are realized with nested grids; the whole computation box is covered with a coarse grid, while a smaller region around the center is covered with a finer grid. A typical model is computed with the nested grid consisting of 643 × 8 cells. Our simulations show that the magnetic field is amplified by the collapse and rotation of the proto-neutron star. We discuss both the numerical techniques employed and astrophysical implications.
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