The model
s15WH07 is a general-relativistic, multi-group radiation-hydrodynamics simulation of a collapsing 15 M☉ star. It ends 597 ms after core bounce, with the shock 867 km out.
Core bounce
The last second of a fifteen-solar-mass star. Its shock stalls 150–200 km out from a newborn neutron star, neutrino-heated bubbles boil up behind it — and then it runs away.
What you are looking at
s15WH07 is a general-relativistic, multi-group radiation-hydrodynamics simulation of a collapsing 15 M☉ star. It ends 597 ms after core bounce, with the shock 867 km out.
Colour follows a model of specific entropy: red where it is low — the shock front, the cool downflows between plumes — blue where it is high. Brightness and opacity follow the gradient of its turbulent part, so bubble walls turn into luminous membranes, after the paper's gradient-enhanced kernel.
Source: SC18 Scientific Visualization & Data Analytics Showcase. The field on this page is procedural: it is styled after the paper's storyline and transfer function and uses none of its data. Times and radii between bounce and the final step are a modelled curve.