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Rapid uniform rotation of proto-neutron stars, hot neutron stars, and neutron star merger remnants: The role of the temperature

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Rapid uniform rotation of proto-neutron stars, hot neutron stars, and neutron star merger remnants: The role of the temperature (EN)
Koliogiannis Koutmiridis, Polychronis Stylianos
info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
Theoretical; Computational (EN)
2022-10-17
Hot and dense nuclear matter and the equation of state is mandatory for studying proto-neutron stars and neutron star merger remnants. The applied equations of state are derived within the momentum-dependent interaction model and state-of-the-art microscopic data, to fulfill the thermodynamic laws. The matter is constructed under the assumptions of finite temperature and beta-equilibrium state, and finite entropy per baryon and varying values of proton fraction. Afterwards, we study the effects of finite temperature and rotation at the mass-shedding limit on the neutron stars properties, including the mass and radius, the moment of inertia, the frequency, the Kerr parameter, the central baryon density, etc. The interplay between the temperature and rotation for proto-neutron stars and neutron star merger remnants may shed light in the construction of the equation of state of nuclear matter and apply robust constraints. (EN)
neutron stars (EN)
nuclear matter (EN)
hot equation of state (EN)
binary neutron star merger remnant (EN)
Annual Symposium of the Hellenic Nuclear Physics Society
English
Hellenic Nuclear Physics Society (HNPS) (EN)
2654-0088
2654-007X
Annual Symposium of the Hellenic Nuclear Physics Society; Τόμ. 28 (2021); 280-285 (EL)
HNPS Advances in Nuclear Physics; Vol. 28 (2021): HNPS2021; 280-285 (EN)
Πνευματική ιδιοκτησία (c) 2022 Polychronis Stylianos Koliogiannis Koutmiridis (EL)
http://creativecommons.org/licenses/by-nc-nd/4.0
Hellenic Nuclear Physics Society
Annual Symposium of the Hellenic Nuclear Physics Society
Oral contributions



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