Exploring Many Facets of Core Collapse Supernovas

Supernova explosions are spectacular astronomical phenomena. At the same time, the understanding of the final journey of a massive star after its nuclear fuel has been exhausted is a challenging problem. The outcome of it is a core collapse supernova and the residue may take the form of either a neutron star or a black hole. The core collapse supernova explosion mechanism is being investigated over the last five decades. Still, the detailed theory of a successful supernova explosion is beyond our reach. In most core collapse supernova simulations, the shock stalls after traversing a few hun- dred kilometers. The shock revival by neutrino heating, after hundreds of milliseconds, was investigated in understanding a successful supernova. On the other hand, novel phases of dense matter such as hyperon, quark or Bose condensates of pions and kaons might be formed just after the bounce of the Fe core. Recently, it was shown that a quark-hadron phase transition might trigger a supernova and produce a second neutrino burst. The question is whether other exotic forms of matter such as hyperon matter may lead to such a conclusion or not. Here I discuss our newly constructed hyperon equation of state (EoS) for core collapse supernova simulations and neutron stars. This is the first supernova EoS involving hyperons which is compatible with the recently measured 2 solar M neutron star. Furthermore I describe the role of hyperon matter on supernova simulations and neutrino signal. Finally I discuss the metastability of the protoneutron star and its connection to the fate of SN1987A.