Bayesian reconstruction of nuclear matter parameters from the equation of state of neutron star matter. (arXiv:2110.15776v2 [nucl-th] UPDATED)
<a href="http://arxiv.org/find/nucl-th/1/au:+Imam_S/0/1/0/all/0/1">Sk Md Adil Imam</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Patra_N/0/1/0/all/0/1">N. K. Patra</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Mondal_C/0/1/0/all/0/1">C. Mondal</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Malik_T/0/1/0/all/0/1">Tuhin Malik</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Agrawal_B/0/1/0/all/0/1">B. K. Agrawal</a>

The nuclear matter parameters (NMPs), those underlie in the construction of
the equation of state (EoS) of neutron star matter, are not directly
accessible. The Bayesian approach is applied to reconstruct the posterior
distributions of NMPs from the EoS of neutron star matter. The constraints on
lower-order parameters as imposed by the finite nuclei observables are
incorporated through appropriately chosen prior distributions. The calculations
are performed with two sets of pseudo data on the EoS whose true models are
known. The median values of second or higher order NMPs show sizeable
deviations from their true values and associated uncertainties are also larger.
The sources of these uncertainties are intrinsic in nature, identified as (i)
the correlations among various NMPs and (ii) the variations in the EoS of
symmetric nuclear matter, symmetry energy, and the neutron-proton asymmetry in
such a way that the neutron star matter EoS remain almost unaffected.

The nuclear matter parameters (NMPs), those underlie in the construction of
the equation of state (EoS) of neutron star matter, are not directly
accessible. The Bayesian approach is applied to reconstruct the posterior
distributions of NMPs from the EoS of neutron star matter. The constraints on
lower-order parameters as imposed by the finite nuclei observables are
incorporated through appropriately chosen prior distributions. The calculations
are performed with two sets of pseudo data on the EoS whose true models are
known. The median values of second or higher order NMPs show sizeable
deviations from their true values and associated uncertainties are also larger.
The sources of these uncertainties are intrinsic in nature, identified as (i)
the correlations among various NMPs and (ii) the variations in the EoS of
symmetric nuclear matter, symmetry energy, and the neutron-proton asymmetry in
such a way that the neutron star matter EoS remain almost unaffected.

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