Constraints on Neutron Star Radii Based on Chiral Effective Field Theory Interactions

被引：315

作者：

Hebeler, K. ^{[1
]}

Lattimer, J. M. ^{[2
]}

Pethick, C. J. ^{[3
,4
]}

Schwenk, A. ^{[1
,5
,6
]}

机构：

[1] TRIUMF, Vancouver, BC V6T 2A3, Canada

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

[3] Niels Bohr Inst, Niels Bohr Int Acad, DK-2100 Copenhagen O, Denmark

[4] NORDITA, SE-10691 Stockholm, Sweden

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

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

来源：

PHYSICAL REVIEW LETTERS | 2010年 / 105卷 / 16期

基金：

加拿大自然科学与工程研究理事会;

关键词：

EQUATION-OF-STATE; NUCLEAR-MATTER; MODELS; DENSITIES;

D O I：

10.1103/PhysRevLett.105.161102

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

We show that microscopic calculations based on chiral effective field theory interactions constrain the properties of neutron-rich matter below nuclear densities to a much higher degree than is reflected in commonly used equations of state. Combined with observed neutron star masses, our results lead to a radius R = 9.7-13.9 km for a 1.4M(circle dot) star, where the theoretical range is due, in about equal amounts, to uncertainties in many-body forces and to the extrapolation to high densities.

引用

页数：4

共 32 条

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[Anonymous], ARXIV10064062

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