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- W3122209580 abstract "Based on the distribution of tidal deformabilities and component masses of binary neutron star merger GW170817, the parametric equation of state (EOS) is employed to probe the nuclear symmetry energy and the properties of the neutron star. To obtain a proper distribution of the parameters of the EOS that is consistent with the observation, Bayesian analysis is used and the constraints of causality and maximum mass are considered. From this analysis, it is found that the symmetry energy and pressure at twice the saturation density of nuclear matter can be constrained within $$E_{sym}(2{rho _{0}}) = 34.5^{+20.5}_{-2.3}$$ MeV and $$P (2{rho _{0}}) = 3.81^{+1.18}_{-2.32}times 10^{34}$$ dyn cm $$^{-2}$$ at 90% credible level, respectively. Moreover, the constraints on the radii and dimensionless tidal deformabilities of canonical neutron stars are also demonstrated through this analysis, and the corresponding constraints are 10.80 km $$le R_{1.4} le $$ 13.20 km and $$133 le Lambda _{1.4} le 686$$ at 90% credible level, with the most probable value of $$bar{R}_{1.4}$$ = 12.60 km and $$bar{Lambda }_{1.4}$$ = 500, respectively. With respect to the prior, our result (posterior result) prefers a softer EOS, corresponding to a lower expected value of symmetry energy, a smaller stellar radius, and a smaller tidal deformability." @default.
- W3122209580 created "2021-02-01" @default.
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- W3122209580 creator A5063063397 @default.
- W3122209580 creator A5071957113 @default.
- W3122209580 date "2021-01-01" @default.
- W3122209580 modified "2023-10-16" @default.
- W3122209580 title "Constraining the nuclear symmetry energy and properties of the neutron star from GW170817 by Bayesian analysis" @default.
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- W3122209580 doi "https://doi.org/10.1140/epja/s10050-021-00342-w" @default.
- W3122209580 hasPublicationYear "2021" @default.
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