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  • An animation of a simulation of a 40-solar-mass progenitor star first exploding vigorously and then giving birth to a black hole after ~1.76 seconds after bounce. This movie also follows the post-black-hole formation epoch to 8.8 seconds after bounce. Graphics: Joe Insley/ALCF; Publication: A. Burrows et al. 2023 - "Black-Hole Formation Accompanied by the Supernova Explosion of a 40-Msun Progenitor".

  • An animation of the results of a state-of-the-art 3D simulation of supernova explosion and neutron-star birth. There is a Techno accompaniment in sound. Highlighted among others things is the deep core that is shrinking after explosion due to neutrino cooling and deleptonization on its way to becoming a cold, compact neutron star. In evidence is inner proto-neutron star convection, perhaps the site of magnetic dynamo action that can turn a pulsar into a magnetar. The final frames are of the blast wave moving at ~10,000 km/s that cocoons the newly-birthed neutron star. (Credit: the Princeton Supernova Theory group; Graphics: Joe Insley/ALCF; Publication: A. Burrows et al. 2020). The sphere in the close-up is an isodensity surface at 109.5 gm/cc colored by Ye.

  • Same as above, but with an orchestral accompaniment. An animation of the results of a state-of-the-art 3D simulation. The YouTube video can be found at: https://www.youtube.com/watch?v=0DSk1wPc_cE .

  • Tracer particles sourced in the proto-neutron-star convection region for a 25-solar-mass model, turbulence interior to the shock. The outer sphere is an isodensity surface at 1011 gm/cc colored by Ye.

  • Tracer particles sourced in the core, showing the PNS and turbulence interior to the shock. The PNS is an isodensity surface, colored by Ye.

  • Tracer particles depicting infall, turbulence, and explosion of a 19-solar-mass progenitor in 3D The inner PNS is painted in Ye and the trajectiries are painted in entropy.

  • Explosion of a 25-solar-mass progenitor in 3D, using the latest implementation of Fornax and plotting isoentropy contours painted with Ye.

  • Explosion of a higher-resolution 19-solar-mass progenitor in 3D using the state-of-the-art simulation code Fornax. Plotted are isoentropy surfaces colored by electron fraction, Ye. The gray veil is the shock surface.

  • Explosion of a 16-solar-mass progenitor in 3D, using the latest implementation of Fornax, but this time plotting the electron fraction, Ye.

  • Explosion of a 9-solar-mass progenitor in 3D, using the latest implementation of Fornax and rendering entropy.

  • Merging of two neutron stars, using the WhiskyTHC code of D. Radice and collaborators.

  • Pathline trajectories during stalled-shock phase.

  • Shock response to rising bubbles and the onset of explosion.

  • 2D slice of the same (just above) 3D explosion, using CASTRO and simple transfer.

  • Rayleigh-Taylor test of the Fornax code, using 512x512x1024 Cartesian zoning.

  • A rotating camera view of a 3D supernova explosion. Note the emergence of the neutron star.

  • A rotating camera view of a frozen anisotropic entropy structure behind the shock.

  • A rotating camera view of a instantaneous heating rate in the gain region behind the stalled shock.

  • Two movies of the same explosion, one for an isoentropy surface and the other employing volume-rendering. The latter reveals the presence and rotation of the residual neutron star.

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    Updated on: October 31, 2019