Neutrinos in supernova evolution and nucleosynthesis

          @misc{ scivideos_PIRSA:11060028,
            doi = {10.48660/11060028},
            url = {https://pirsa.org/11060028},
            author = {Martnez-Pinedo, Gabriel},
            keywords = {Particle Physics},
            language = {en},
            title = {Neutrinos in supernova evolution and nucleosynthesis},
            publisher = {Perimeter Institute for Theoretical Physics},
            year = {2011},
            month = {jun},
            note = {PIRSA:11060028 see, \url{https://scivideos.org/index.php/pirsa/11060028}}
          }
          

Abstract

Massive accretion disks may form from the merger of neutron star (NS)-NS or black hole-NS binaries, or following the accretion-induced collapse (AIC) of a white dwarf. These disks, termed `hyper-accreting' due to their accretion rates up to several solar masses per second, may power the relativistic jets responsible for short duration gamma-ray bursts. Using 1D time-dependent calculations of hyper-accreting disks, I show that a generic consequence of the disk's late-time evolution is the development of a powerful outflow, powered by viscous heating and the recombination of free nuclei into Helium. These outflows - in additional to any material dynamically-ejected during the merger - synthesize heavy radioactive elements as they expand into space. Nuclear heating from the r-process is not yet incorporated in merger simulations, yet has important consequences both for the dynamics of late `fall-back' accretion and in powering a supernova-like transient (`kilonova') 1 day following the merger or AIC.