Constraining a relativistic mean field model using neutron star mass-radius measurements I: nucleonic models

被引：23

作者：

Huang, Chun ^{[1
,2
,3
]}

Raaijmakers, Geert ^{[4
]}

Watts, Anna L. ^{[2
]}

Tolos, Laura ^{[5
,6
,7
]}

Providencia, Constanca ^{[8
]}

机构：

[1] Cent China Normal Univ, Phys Dept, Luoyu Rd, Wuhan 430030, Peoples R China

[2] Univ Amsterdam, Anton Pannekoek Inst Astron, Sci Pk 904, NL-1090 GE Amsterdam, Netherlands

[3] Washington Univ, Phys Dept, One Brookings Dr, St Louis, MO 63130 USA

[4] Univ Amsterdam, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands

[5] Campus UAB, Inst Space Sci ICE CSIC, Carrer Can Magrans, E-08193 Barcelona, Spain

[6] Inst Estudis Espacials Catalunya IEEC, E-08034 Barcelona, Spain

[7] Frankfurt Inst Adv Studies, Ruth Moufang Str 1, D-60438 Frankfurt, Germany

[8] Univ Coimbra, Dept Phys, CFisUC, P-3004516 Coimbra, Portugal

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2024年 / 529卷 / 04期

关键词：

dense matter; equation of state; stars: neutron; X-rays: general; EQUATION-OF-STATE; DENSE MATTER; GRAVITATIONAL-WAVE; NUCLEAR-EQUATION; PSR J0740+6620; NICER DATA; MULTIMESSENGER; INFERENCE; IMPACT; ENERGY;

D O I：

10.1093/mnras/stae844

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Measurements of neutron star mass and radius or tidal deformability deliver unique insight into the equation of state (EOS) of cold dense matter. EOS inference is very often done using generalized parametric or non-parametric models, which deliver no information on composition. In this paper, we consider a microscopic nuclear EOS model based on a field theoretical approach. We show that current measurements from NICER and gravitational wave observations constrain primarily the symmetric nuclear matter EOS. We then explore what could be delivered by measurements of mass and radius at the level anticipated for future large-area X-ray timing telescopes. These should be able to place very strong limits on the symmetric nuclear matter EOS, in addition to constraining the nuclear symmetry energy that determines the proton fraction inside the neutron star.

引用

页码：4650 / 4665

页数：16

共 113 条

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