Mass ejection in non-rotating failed supernovae

by Rodrigo Fernandez

Thursday 24 Nov 2022, 13:15 → 14:15 Europe/Stockholm

Albano 3: 6228 - Mega (22 seats) (Albano Building 3)

The core-collapse of a slowly-rotating massive star that fails to explode results in the formation of a black hole (BH). Below the pair-instability threshold, a protoneutron star phase always precedes BH formation, with a corresponding reduction in the total gravitational mass due to neutrino emission. The ensuing deviation from hydrostatic equilibrium in the outer layers of the star results in the ejection of a small amount of mass with much lower energies than in successful supernovae. The mass and velocity of the ejecta depend on properties of the core and envelope of the progenitor. I'll discuss an exploration of this mechanism over a wide range of stellar progenitors using spherically-symmetric hydrodynamic simulations, focusing on the effect of the dense-matter equation of state and spatial resolution on the ejecta properties, expected electromagnetic counterparts, and upper limits to the mass of the BH remnant.