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Many calculations of the neutron star (NS) equation of state (EOS) have been performed over the years. Recent observations of NSs have begun to play an important role in finding… Click to show full abstract
Many calculations of the neutron star (NS) equation of state (EOS) have been performed over the years. Recent observations of NSs have begun to play an important role in finding the realistic EOS. In this paper, we compare mass–radius relations derived from various EOSs with observational data of NSs. In addition, we adjust EOSs to be consistent with observational data from NSs and employ Bayesian statistical analyses to obtain constraints on the EOS. Our results show that the EOS needs to be softened in the medium density region (2ρ0–4ρ0, where ρ0 is the saturation density) and to have a rapid change of stiffness around an energy density of ∼ 650 MeV/fm3.
Journal Title: Modern Physics Letters A
Year Published: 2017
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