Impact of the Nuclear Equation of State on the Stability of Hybrid Neutron Stars

Abstract

We construct a set of equations of state (EoS) of dense and hot matter with a 1st order phase transition from a hadronic system to a deconfined quark matter state. In this two-phase approach, hadrons are described using the relativistic mean field theory with different parametrisations and the deconfined quark phase is modeled using vBag, a bag-type model extended to include vector interactions as well as a simultaneous onset of chiral symmetry restoration and deconfinement. This feature results in a non-trivial connection between the hadron and quark EoS, modifying the quark phase beyond its onset density. We find that this unique property has an impact on the predicted hybrid (quark core) neutron star mass--radius relations.

13 pages, 9 figures, conference proceedings of CSQCD 7. arXiv admin note: text overlap with arXiv:1802.03214

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• Exploring thermal effects of the hadron-quark matter transition in neutron star mergers
• Vector dark boson mediated feeble interaction between fermionic dark matter and strange quark matter in quark stars
• Constraints on Density Dependent MIT Bag Model Parameters for Quark and Hybrid Stars
• Compactness in the Thermal Evolution of Twin Stars
• A Detailed Analysis of the Special Points on $M-R$ Solutions of Hybrid (Twin) Stars
• Effects of dark boson mediated feeble interaction between dark matter (DM) and quark matter on $f$-mode oscillation of DM admixed quark stars