CCSN / s15WH07

Core bounce

CoreCollapse

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.

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What you are looking at

Entropy in colour.
Its gradient in light.

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.

The picture

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.

The numbers

Grid
633³ at 3.96 km
Time steps
1077
Data
1.1 TB

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.