Abstract
The properties of compact stars and in particular the existence of twin star solutions are investigated within an effective model that is constrained by lattice QCD thermodynamics. The model is modified at large baryon densities to incorporate a large variety of scenarios of first order phase transitions to a phase of deconfined quarks. This is achieved by matching two different variants of the bag model equation of state, in order to estimate the role of the Bag model parameters on the appearance of a second family of neutron stars. The produced sequences of neutron stars are compared with modern constrains on stellar masses, radii, and tidal deformability from astrophysical observations and gravitational wave analyses. It is found that those scenarios in our analysis, in which a third family of stars appeared due to the deconfinement transition, are disfavored from astrophysical constraints.
Highlights
It is presumed that neutron stars (NS) can contain deconfined quark matter due to the high densities achieved in their interiors and might play a decisive role along with both low and high energy nuclear physics in the exploration of the strong interaction and the Quantum Chromodynamics (QCD) phase diagram
The viability of twin star solutions due to a sharp phase transition to deconfined quark matter was studied in the context of the CMF model
The CMF model is a new type of effective description of QCD thermodynamics which includes the effects of chiral symmetry restoration as well as a coexistence between quarks and hadrons
Summary
It is presumed that neutron stars (NS) can contain deconfined quark matter due to the high densities achieved in their interiors and might play a decisive role along with both low and high energy nuclear physics in the exploration of the strong interaction and the Quantum Chromodynamics (QCD) phase diagram. In context of the QCD phase diagram, astrophysical searches for signals of phase transition in compact star matter by detecting twin stars or finding a star from a third family of compact stars are of particular interest. Both these cases imply the existence of an isolated branch of stable compact star configurations in the mass radius diagram. The EoS for compact stars is often calculated on a basis of nuclear interaction models [27,28], including additional hyperonic degrees of freedom [29,30,31,32,33] and models based
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