Equation of State Constraints from Nuclear Physics, Neutron Star Masses, and Future Moment of Inertia Measurements

被引：58

作者：

Greif, S. K. ^{[1
,2
]}

Hebeler, K. ^{[1
,2
]}

Lattimer, J. M. ^{[3
]}

Pethick, C. J. ^{[4
,5
,6
]}

Schwenk, A. ^{[1
,2
,7
]}

机构：

[1] Tech Univ Darmstadt, Inst Kernphys, D-64289 Darmstadt, Germany

[2] GSI Helmholtzzentrum Schwerionenforsch GmbH, ExtreMe Matter Inst EMMI, D-64291 Darmstadt, Germany

[3] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA

[4] Univ Copenhagen, Niels Bohr Int Acad, Niels Bohr Inst, Blegdamsvej 17, DK-2100 Copenhagen O, Denmark

[5] KTH Royal Inst Technol, NORDITA, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden

[6] Stockholm Univ, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden

[7] Max Planck Inst Kernphys, Saupfercheckweg 1, D-69117 Heidelberg, Germany

来源：

ASTROPHYSICAL JOURNAL | 2020年 / 901卷 / 02期

关键词：

Neutron stars; Nuclear astrophysics; ROTATING RELATIVISTIC STARS; MATTER; FORCES;

D O I：

10.3847/1538-4357/abaf55

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We explore constraints on the equation of state (EOS) of neutron-rich matter based on microscopic calculations up to nuclear densities and observations of neutron stars. In a previous work we showed that predictions based on modern nuclear interactions derived within chiral effective field theory and the observation of two-solar-mass neutron stars result in a robust uncertainty range for neutron star radii and the EOS over a wide range of densities. In this work we extend this study, employing both the piecewise polytrope extension from Hebeler et al. as well as the speed of sound model of Greif et al., and show that moment of inertia measurements of neutron stars can significantly improve the constraints on the EOS and neutron star radii.

引用

页数：9

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