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Compact stars consisting of strange quark matter and strange matter with admissible dark matter are studied by solving the Tolman‐Oppenheimer‐Volkoff equations for two fluids interacting only by gravity, with the dark‐matter EoS obtained by means of galaxy rotation curves. The properties of these stars are explored by means of the modeling of their mass‐radius relations and gravitational redshifts.
In this contribution, we study the nature of the quantum chromodynamics (QCD) phase transition in hybrid compact stars. In our approach, we consider a microscopic hadron–quark hybrid equation of state (EoS) to describe the structure of compact stars composed of a quark core and a hadronic shell assuming a structural first‐order phase transition at their interface. Our primary purpose in this contribution...
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