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The high temperatures reached in a proto-neutron star or during the post-merger phase of a binary neutron star coalescence lead to non-negligible thermal effects on the equation of state (EOS) of dense nuclear matter.
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H. D. Thi, C. Mondal, F. Gulminelli, The Nuclear Matter Density Functional under the Nucleonic Hypothesis, Universe 7 (10) (2021) 373 · 2021
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O. E. Andersen, S. Zha, A. da Silva Schneider, A. Betranhandy, S. M. Couch, E. P. O’Connor, Equation-of-state dependence of gravitational waves in core-collapse supernovae, Astrophys. J. 923 (2) (2021) 201 · 2021
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P. Char, C. Mondal, F. Gulminelli, M. Oertel, Generalized description of neutron star matter with a nucleonic relativistic density functional, Phys. Rev. D 108 (10) (2023) 103045 · 2023
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C. A. Raithel, V. Paschalidis, Influence of stellar compactness on finite-temperature effects in neutron star merger simulations, Phys. Rev. D 108 (2023) 083029 · 2023
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J. Fields, A. Prakash, M. Breschi, D. Radice, S. Bernuzzi, A. da Silva Schneider, Thermal Effects in Binary Neutron Star Mergers, Astrophys. J. Lett. 952 (2) (2023) L36 · 2041
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