Speaker
Description
Similar to the crossover phase transition in lattice QCD, at high temperature and small baryon chemical potential, recently, the structure of neutron stars have been studied with a crossover equation of state to model a smooth transition from a pure neutron matter to massless quarks [1]. The switch function, that guides the crossover, was constrained in order to reproduce neutron stars up to about two solar masses. Afterwards, such a study has been extended by considering the relevance of color superconducting massless quarks in the cold dense matter [2]. In this contribution, we investigate the hadron to quark crossover transition by means of an equation of state which incorporates hadronic matter, composed by nucleons, hyperons and
[1] J.I. Kapusta, T. Welle, Phys. Rev. C 104, L012801 (2021)
[2] D. Blaschke, E.-O. Hanu, S. Liebing, Phys. Rev. C 105, 035804 (2022)
session | H. Equation of State and Neutron Stars |
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