We investigate remnant neutron star masses ( in particular , the minimum allowed mass ) by performing advanced stellar evolution calculations and neutrino-radiation hydrodynamics simulations for core-collapse supernova explosions .
We find that , based on standard astrophysical scenarios , low-mass carbon-oxygen cores can have sufficiently massive iron cores that eventually collapse , explode as supernovae , and give rise to remnant neutron stars that have a minimum mass of 1.17 M _ { \odot } — compatible with the lowest mass of the neutron star precisely measured in a binary system of PSR J0453+1559 .