Bayesian inference of the skewness parameter of supra-dense nuclear matter from energetic heavy-ion reactions. (arXiv:2001.03669v1 [nucl-th])

<a href="http://arxiv.org/find/nucl-th/1/au:+Xie_W/0/1/0/all/0/1">Wen-Jie Xie</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Li_B/0/1/0/all/0/1">Bao-An Li</a>

Within the Bayesian framework using available constraining bands on the

pressure in symmetric nuclear matter (SNM) derived earlier by others in the

density range of 1.3$rho_0$ to 4.5$rho_0$ from kaon production and nuclear

collective flow data in energetic heavy-ion collisions, we infer the posterior

probability distribution functions (PDFs) of SNM incompressibility $K_0$ and

skewness $J_0$ using uniform prior PDFs for them in the ranges of $220leq

K_0leq 260$ MeV and $-800leq J_0leq 400$ MeV. The 68% posterior credible

boundaries around the most probable values of $K_0$ and $J_0$ are found to be

222$pm$2 MeV and -215$pm$20 MeV, respectively, much narrower than their prior

ranges widely used currently in the literature and are consistent with the

results of a recent Bayesian analysis of neutron star properties constrained by

available X-ray and gravitational wave observations.

Within the Bayesian framework using available constraining bands on the

pressure in symmetric nuclear matter (SNM) derived earlier by others in the

density range of 1.3$rho_0$ to 4.5$rho_0$ from kaon production and nuclear

collective flow data in energetic heavy-ion collisions, we infer the posterior

probability distribution functions (PDFs) of SNM incompressibility $K_0$ and

skewness $J_0$ using uniform prior PDFs for them in the ranges of $220leq

K_0leq 260$ MeV and $-800leq J_0leq 400$ MeV. The 68% posterior credible

boundaries around the most probable values of $K_0$ and $J_0$ are found to be

222$pm$2 MeV and -215$pm$20 MeV, respectively, much narrower than their prior

ranges widely used currently in the literature and are consistent with the

results of a recent Bayesian analysis of neutron star properties constrained by

available X-ray and gravitational wave observations.

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