Berlin 2005 – scientific programme
Parts | Days | Selection | Search | Downloads | Help
HK: Physik der Hadronen und Kerne
HK 20: Kern- und Teilchen-Astrophysik
HK 20.1: Talk
Monday, March 7, 2005, 14:00–14:15, TU MA144
Neutrino transport in proto neutron stars — •Jens Berdermann1, David Blaschke2,3, and Hovik Grigorian1,4 — 1Fachbereich Physik, Universität Rostock, Germany — 2Bogoliubov Laboratory of Theoretical Physics, > Joint Institute for Nuclear Research, 141980, Dubna, Russia — 3Fakultät für Physik, Universität Bielefeld, > D-33615 Bielefeld, Germany — 4Department of Physics, Yerevan State University, 375025 > Yerevan, Armenia
> Proto neutron stars (PNS) are created after type II supernova explosions > with initial temperatures up to 40 MeV. > In such a hot, dense environment, as long as the > temperature T ≥ 1 MeV, the neutrino mean free path > is much smaller than the star radius R ∼ 10 km and the > PNS is practically opac for neutrinos. > The neutrino transport in this neutrino trapping regime > is described in the equilibrium diffusion approximation, > which gives a satisfactory description for the limiting cases of > trapping > (Yl ≈ 0.38, s ≃ 1, T ≥ 1÷3 MeV) > and free radiation (Yν ≈ 0, s ≃ 2, T ≤ 1÷3 > MeV). > We show the advantages and limitations of this approximations and give > an > outlook to effects due to the inclusion of accretion and rotation > of the PNS. > > > Partially supported by DFG Graduiertenkolleg 567 ”Stark korrelierte > > Vielteilchensysteme” at Universität Rostock. > > > > > >