Symmetry energy effects on the properties of hybrid stars

Abstract

Symmetry energy is an important part of the equation of state of isospin asymmetry matter. However, the huge uncertainties of symmetry energy remain at suprasaturation densities, where the phase transitions of strongly interacting matter and the quark matter symmetry energy are likely to be taken into account. In this work, we investigate the properties of symmetry energy by using a hybrid star with the hadron-quark phase transition. The interaction among strange quark matter (SQM) in hybrid stars is based on a 3-flavor NJL model with different vector and isovector channels, while the equation of state (EOS) of the nuclear matter is obtained by considering the ImMDI-ST interaction by varying the parameters x, y, and z. Our results indicate that the various parameters and coupling constants of the interactions from the ImMDI-ST and NJL model can lead to widely different trends for the symmetry energy in the hadron-quark mixed phase and the different onsets of the hadron-quark phase transition. In addition, it has been found that the radii and tidal deformabilities of hybrid stars constrain mostly the density dependence of symmetry energy while the observed maximum masses of hybrid stars constrain mostly the EOS of symmetric nuclear and quark matter.

arXiv admin note: text overlap with arXiv:1905.13175 by other authors

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• A Detailed Analysis of the Special Points on $M-R$ Solutions of Hybrid (Twin) Stars
• Properties of quark matter and hybrid stars from a quasiparticle model
• Properties of quark-matter cores in massive hybrid stars
• Rotating Hybrid Stars with Color-Flavor-Locked Quark Matter
• Speed of sound and polytropic index in QCD matter
• Axion effects on quark matter and quark-matter cores in massive hybrid stars
• Can a hybrid star with constant sound speed parametrization explain the new NICER mass-radius measurements ?
• Isentropic thermodynamics across the hadron-quark mixed phase in a two-phase model with a PNJL quark description