Bayesian analysis of generic hybrid EOS with first-order deconfinement shows mass-gap hybrids require early transition and stiff quark matter, but data favor twins at 1.4 M_sun that exclude them.
Revisiting the Rhoades-Ruffini bound
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abstract
We revisit the derivation of the Rhoades-Ruffini bound on the upper limit for the maximum mass of neutron stars and find that the assumption made there for the onset of an ultimately stiff phase of high-density matter is not stringent. Relaxing this assumption and allowing for an onset of stiff non-nucleonic matter under neutron star constraints at the saturation density or below boost the upper limit of the theoretically possible maximum mass to $4~M_\odot$ or higher, in the mass-gap region between neutron stars and stellar-mass black holes. We provide a fit formula for the dependence of this upper limit on the speed of sound and the onset density of the deconfinement transition.
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Hybrid stars among mass gap objects are excluded by twin stars at $1.4\,M_\odot$
Bayesian analysis of generic hybrid EOS with first-order deconfinement shows mass-gap hybrids require early transition and stiff quark matter, but data favor twins at 1.4 M_sun that exclude them.