Astronomy and Astrophysics – Astrophysics
Scientific paper
2004-08-09
Astronomy and Astrophysics
Astrophysics
4 pages, contribution to Nuclei in the Cosmos VIII, Jul. 19-23, submitted to Nucl. Phys. A
Scientific paper
10.1016/j.nuclphysa.2005.05.016
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.
Liebendoerfer Matthias
Pen U.-L.
Thompson Christopher
No associations
LandOfFree
Approaching the dynamics of hot nucleons in supernovae does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Approaching the dynamics of hot nucleons in supernovae, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Approaching the dynamics of hot nucleons in supernovae will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-358361