Maximum pulsar mass, equation of state and structure of neutron-star cores

6th Nuclear Physics in Astrophysics

物理学;天文学

Haensel, P.^1 ; Zdunik, J.L.^1

N. Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, Warszawa

PL-00-716, Poland^1

关键词: Dense matter;    Equation of state;    Fine tuning;    Hadronic matters;    Neutron stars;    Nuclear matters;    Present situation;    Quark matter;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/665/1/012061/pdf
DOI  :  10.1088/1742-6596/665/1/012061

学科分类：天文学(综合)

来源: IOP

【 摘 要 】

The structure of neutron stars is determined by the equation of state of dense matter in their interiors. Brief review of the equation of state from neutron star surface to its center is presented. Recent discovery of two two-solar-mass pulsars puts interesting constraints on the poorly known equation of state of neutron-star cores for densities greater than normal nuclear matter density. Namely, this equation of state has to be stiff enough to yield maximum allowable mass of neutron stars greater than two solar masses. There are many models of neutron stars cores involving exclusively nucleons that satisfy this constraint. However, for neutron-star models based on recent realistic baryon interaction, and allowing for the presence of hyperons, the hyperon softening of the equation of state yields maximum masses significantly lower than two solar masses. Proposed ways out from this "hyperon puzzle" are presented. They require a very fine tuning of parameters of dense hadronic matter and quark matter models. Consequences for the mass-radius relation for neutron stars are illustrated. A summary of the present situation and possible perspectives/challenges, as well as possible observational tests, are given.