Remnant masses of core collapse supernovae in the jittering jets explosion mechanism
Dmitry Shishkin, Noam Soker
Abstract
ABSTRACT We conduct one-dimensional (1D) stellar evolution simulations of non-rotating stars with initial masses in the range of $11\!-\!48 \, \mathrm{M}_{\odot }$ to the time of core collapse and, using a criterion on the specific angular momentum fluctuations in the inner convective zones, estimate the masses of the neutron star (NS) remnants according to the jittering jets explosion mechanism. From the 1D simulations, we find that several convective zones with specific angular momentum fluctuations of $j_{\rm {conv}} \gtrsim 2.5 \times 10^{15} {\, \rm cm}^2 {\, \rm s}^{-1}$ develop near the edge of the iron core in all models. For this condition for explosion, we find the NS remnant masses to be in the range of $1.3\!-\!1.8 \, \mathrm{M}_\odot$, while if we require twice as large values, i.e. $j_{\rm {conv}} \gtrsim 5 \times 10^{15} {\, \rm cm}^2 {\, \rm s}^{-1}$, we find the NS remnant masses to be in the range of $1.4\!-\!2.8 \, \mathrm{M}_\odot$ (the upper values here might form black holes). Note that in general, the formation of black holes in the jittering jets explosion mechanism requires a rapidly rotating pre-collapse core, while we simulate non-rotating stars.