  General Relativistic Entropic Acceleration (GREA) gives a general framework
in which to study multiple out-of-equilibrium phenomena in the context of
general relativity, like the late accelerated expansion of the universe or the
formation of galaxies and the large scale structure of the universe. Here we
analyze the conditions for collapse of a star of degenerate neutrons in the
presence of entropy production due to the gravitational collapse itself. We
find that the final mass and radius of the neutron star differs from that
obtained with the adiabatic Tolman-Oppenheimer-Volkoff equation by a factor of
order 15\%. We also find that the minimum mass of a neutron star is $\sim
1.1\,M_\odot$ and the maximum mass around $2.4\,M_\odot$. We discuss the
possible implications for the search and interpretation of binary coalescing
systems like neutron stars and neutron star-black holes detectable via their
multimessenger (gravitational and electromagnetic wave) emission upon merging.
