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Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE, Astrophysics, Solar and Stellar Astrophysics, astro-ph.SR,Nuclear Theory, nucl-th
Abstract:
We investigate the post-explosion phase in core-collapse supernovae with 2D
hydrodynamical simulations and a simple neutrino treatment. The latter allows
us to perform 46 simulations and follow the evolution of the 32 successful
explosions during several seconds. We present a broad study based on three
progenitors (11.2 $M_\odot$, 15 $M_\odot$, and 27 $M_\odot$), different
neutrino-heating efficiencies, and various rotation rates. We show that the
first seconds after shock revival determine the final explosion energy, remnant
mass, and properties of ejected matter. Our results suggest that a continued
mass accretion increases the explosion energy even at late times. We link the
late-time mass accretion to initial conditions such as rotation strength and
shock deformation at explosion time. Only some of our simulations develop a
neutrino-driven wind that survives for several seconds. This indicates that
neutrino-driven winds are not a standard feature expected after every
successful explosion. Even if our neutrino treatment is simple, we estimate the
nucleosynthesis of the exploding models for the 15 $M_\odot$ progenitor after
correcting the neutrino energies and luminosities to get a more realistic
electron fraction.
