Speaker
Description
We study the minimal masses and radii of proto-neutron stars during different stages of their evolution.
The main focus lies on the stages directly before the supernova explosion where neutrinos are captured in the core
and the lepton per baryon ratio is approximately $Y_L = 0.4$ and a few seconds after the supernova,
when all neutrinos have left the star.
All equations of state used for this purpose fulfill $\textit{Chiral Effective Field Theory}$ constraints for the binding energy at $T = 0$.
We find for the neutrino-trapped cases higher minimal masses than for the cases when neutrinos are not in the system anymore.
Thermal effects, characterized by a higher constant entropy per baryon, further elevate the minimal mass. We additionally study the minimal mass dependence on the lepton fraction, which follows a similar curve for all equations of state studied.
The masses for the cases studied all lie between $M_{min}$ = $0.11$$M_{\odot}$ and $0.85$ $M_{\odot}$. Hence, proto-neutron stars can exhibit higher minimal masses than their cold, catalyzed form during all stages of their evolution.
