Approaching the dynamics of hot nucleons in supernovae

Abstract

All recent numerical simulations agree that stars in the main sequence mass range of 9-40 solar masses do not produce a prompt hydrodynamic ejection of the outer layers after core collapse and bounce. Rather they suggest that stellar core collapse and supernova explosion are dynamically distinct astrophysical events, separated by an unspectacular accretion phase of at least ~40 ms duration. As long as the neutrinospheres remain convectively stable, the explosion dynamics is determined by the neutrons, protons, electrons and neutrinos in the layer of impact-heated matter piling up on the protoneutron star. The crucial role of neutrino transport in this regime has been emphasized in many previous investigations. Here, we search for efficient means to address the role of magnetic fields and fluid instabilities in stellar core collapse and the postbounce phase.

arXiv comment4 pages, contribution to Nuclei in the Cosmos VIII, Jul. 19-23, submitted to Nucl. Phys. A

References in corpus (10)

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Cited by in corpus (5)

• Magnetorotationally driven Supernovae as the origin of early galaxy $r$-process elements?
• A simple parameterization of the consequences of deleptonization for simulations of stellar core collapse
• MAGMA: a 3D, Lagrangian magnetohydrodynamics code for merger applications
• Stability of the Accretion Flows with Stalled Shocks in Core-Collapse Supernovae
• Stellar evolution of massive stars at very low metallicities