A study of the composition and properties of neutron stars and proto-neutron stars is presented,
based on a relativistic mean-field model. The baryonic matter equation of state at zero and finite
temperatures is computed within the FSU2H* model, which has been updated according to a
recent analysis for the Ξ baryon nuclear potential. The finite temperature EoS and composition of
matter are computed at constant temperature. It is found that temperature effects are significant
and cannot be well reproduced with simple approximations, as the usually adopted Γ - law. This
can have a strong impact on the neutron star observables obtained as outputs of complicated
relativistic simulations, such as the mass, radius and tidal deformability.
Equation of state of hot hyperonic neutron star core
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Published on:
June 19, 2023
Abstract
DOI: https://doi.org/10.22323/1.419.0027
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Copyright owned by the author(s) under the term of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.