Finite-temperature equation of state with hyperons

Abstract

We present the novel finite-temperature FSU2H${}^{\ast }$ equation-of-state model that covers a wide range of temperatures and lepton fractions for the conditions in proto-neutron stars, neutron star mergers and supernovae. The temperature effects on the thermodynamical observables and the composition of the neutron star core are stronger when the hyperonic degrees of freedom are considered. We pay a special attention to the temperature and density dependence of the thermal index in the presence of hyperons and conclude that the true thermal effects cannot be reproduced with the use of a constant $\Gamma$ law.

8 pages, 5 figures, contribution to the proceedings of the XVth Quark confinement and the Hadron spectrum conference (ConfXV), University of Stavanger, August 1-6, 2022

References in corpus (11)

• GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
• Shapiro delay measurement of a two solar mass neutron star
• A Massive Pulsar in a Compact Relativistic Binary
• PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter
• A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation
• A NICER View of the Massive Pulsar PSR J0740+6620 Informed by Radio Timing and XMM-Newton Spectroscopy
• Neutron Stars and the Nuclear Equation of State
• Equation of State for Nucleonic and Hyperonic Neutron Stars with Mass and Radius Constraints
• The Equation of State for the Nucleonic and Hyperonic Core of Neutron Stars
• Constraints on ${\Xi }^{-}$ nuclear interactions from capture events in emulsion
• The Radius of PSR J0740+6620 from NICER and XMM-Newton Data

Cited by in corpus (1)

• Temperature and Strong Magnetic Field Effects in Dense Matter