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Open AccessArticle

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

1
Institute of Theoretical Physics, University of Wrocław, 50-204 Wroclaw, Poland
2
Department of Physics and Astronomy, California State University Long Beach, 1250 Bellflower Blvd., Long Beach, CA 90840, USA
*
Author to whom correspondence should be addressed.
Universe 2019, 5(8), 186; https://doi.org/10.3390/universe5080186
Received: 8 May 2019 / Revised: 7 August 2019 / Accepted: 8 August 2019 / Published: 12 August 2019
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. View Full-Text
Keywords: dense matter; quantum chromodyamics; neutron stars; bag model; Dyson–Schwinger equations dense matter; quantum chromodyamics; neutron stars; bag model; Dyson–Schwinger equations
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Cierniak, M.; Fischer, T.; Bastian, N.-U.; Klähn, T.; Salinas, M. Impact of the Nuclear Equation of State on the Stability of Hybrid Neutron Stars. Universe 2019, 5, 186.

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