Supemovae neutrinos

Neutrino oscillations in the weak matter effect regime have been discussed extensively before [1-13], in particular, for the solar and supemovae neutrinos propagating in the matter of the Earth. The previous work has been done mainly in the approximation of constant density profile which consists of several layers with constant density. 

The above models are all rather unsatisfactory, because they involve somewhat arbitrary assumptions about the time-dependence of the cosmic-ray flux and spectrum and because they predict a secondary-like behaviour for Be and B abundances, whereas the overall trend indicated by the data is more like a primary one and there are the energetic difficulties pointed out above. In the case of nB, there is a possible primary mechanism for stellar production in supemovae by neutrino spallation processes (Woosley et al. 1990 Woosley Weaver 1995), but the primary-like behaviour of beryllium in metal-poor stars, combined with a constant B/Be ratio of about 20 fully consistent with cosmic-ray spallation (Garcia Lopez et al. 1998) in the absence of any known similar process for Be, indicates that this does not solve the problem unless a primary process can be found for Be as well. Indeed,... 

Here we focus on some recent highlights in both core collapse and thermonuclear supernova studies, which became possible mainly due to increasingly accurate radiation hydrodynamic calculations with a detailed treatment of neutrino processes. We also briefly describe recent success of asymmetric SN simulations (2D magneto-rotational collapse). Next we focus on recently established link between GRB explosions and energetic type Ibc supemovae (hypernovae) and discuss recent ideas on the GRB progenitors. We hypothesize that different core collapse outcomes may lead to the formation of different classes of GRBs. 

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