Neutron stars are unique laboratories to probe matter in extreme conditions that cannot be currently reproduced on Earth. The determination of their equation of state (EoS) is a challenge, but it is particularly important since it allows to relate different global neutron-star properties and to link the prediction of astrophysical observables to microphysical properties of dense matter.
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The calculation of the equation of state (EOS) of nuclear matter beyond saturation density (n_sat) remains an open research problem. However, observations of neutron stars have proven crucial to the study of matter at these higher densities, especially since the detection of gravitational waves from binary neutron star mergers by LIGO and the determination of simultaneous mass-radius contours...
The equation of state (EOS) of dense matter plays a key role in the evolution of the proto-neutron star (PNS) and the dynamics of the core-collapse supernova (CCSN) explosion. We present new EOS tables based on the model of Huth et al (2021), that consider constraints from nuclear theory calculations, experiments, and astrophysical observations. In this study, we systematically vary nuclear...
