Magnetorotational Core-Collapse Supernovae

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… in Three Dimensions (xz-slice)

This movie shows the time-evolution of the shock wave that is created when the core of a rapidly rotating, strongly magnetized massive star collapses to a proto-neutron star. The dynamics are dominated by the ultra-strong magnetic field (~10^16G) that is build up during and shortly after the collapse. A prompt jet-like explosion is foiled by a spiraling MHD kink instability that disrupts the jet. Subsequently magnetic fields continue to dominate as funnels of highly magnetized, launched from the proto-neutron star, advance the shock front outwards in a highly asymmetric fashion. The different colors correspond to gas of different temperature (the variable shown is “specific entropy”, which is closely related to temperature). Blue corresponds to the coldest gas, green is hotter gas, and yellow and red are the hottest gas. The movie depicts a 2D simulation on the left, and the corresponding meridional slice from a 3D simulation on the right.

This movie was generated by the Simulating eXtreme Spacetimes (SXS) project. The simulation work was led by Philipp Moesta at Caltech and the movie was rendered by Sherwood Richers, also at Caltech.

Read also: To Supernova or Not to Supernova: A 3-D Model of Stellar Core Collapse 

Written by physicsgg

May 6, 2014 at 12:57 pm


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