Spherical configuration of a super-dense hot compact object with   particular EoS
  The equation of state (EoS) $P = P (\rho, ...)$ -- pressure as a function of density and other thermodynamical quantities -- is what generates particularities of mass--radius distribution $M (R)$ for super--dense compact stellar bodies, the remnants of cosmic cataclysms. In view of recent nuclear experiments, we propose one particular EoS, which admits the critical state characterized by density $\rho_c$ and temperature $T_c$, and which under certain conditions permits a radial distribution of the super--dense matter in "liquid" phase. We establish such conditions and demonstrate that a stable configuration is indeed possible (only) for temperatures smaller than the critical one. Using Tolman--Oppenheimer--Volkoff equations for hydrostatic equilibrium, we derive the mass--radius relation for the super--dense compact objects with masses smaller than the Sun, $M \ll M_{\odot}$. The obtained results are within the constraints established by both heavy--ion collision experiments and theoretical studies of neutron--rich matter. 
E.P. Tito, V.I. Pavlov
astro-ph.HE nucl-th