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HK: Fachverband Physik der Hadronen und Kerne
HK 32: Nuclear Astrophysics IV
HK 32.4: Vortrag
Mittwoch, 12. März 2025, 16:45–17:00, SR 0.03 Erw. Physik
Determining proto-neutron stars’ minimal mass with chirally constrained nuclear equations of state — •Selina Kunkel, Stephan Wystub, and Jürgen Schaffner-Bielich — Institut für Theoretische Physik, Goethe Universität, Frankfurt am Main, Germany
The minimal masses and radii of proto-neutron stars during different stages of their evolution are investigated. We focus on two stages, directly after the supernova shock wave moves outwards, when neutrinos are still captured in the core and the lepton per baryon ratio is fixed to YL = 0.4, and a few seconds afterwards, when all neutrinos have left the star. We find for the neutrino-trapped case higher minimal masses than for the case when neutrinos have left the proto-neutron star. Thermal effects, here in the form of a given constant entropy per baryon s, have a smaller effect on increasing the minimal mass. The minimal proto-neutron star mass for the first evolutionary stage with YL = 0.4 and s = 1 amounts to Mmin ∼ 0.62M⊙ and for the stage without neutrinos and s = 2 to Mmin ∼ 0.22M⊙ rather independent on the nuclear equation of state used. We demonstrate that there is a universal relation for the increase of the proto-neutron star minimal mass with the lepton fraction for all nuclear equations of state used. We discuss a possible extension of our investigation for studying the appearance of color superconducting phases during proton-neutron star evolution.
Keywords: Proto-Neutron Star; Equation of State; Chiral Effective Field Theory; Minimal mass; Neutrinos