PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter

被引：1135

作者：

Miller, M. C. ^{[1
,2
]}

Lamb, F. K. ^{[3
,4
,5
]}

Dittmann, A. J. ^{[1
,2
]}

Bogdanov, S. ^{[6
]}

Arzoumanian, Z. ^{[7
]}

Gendreau, K. C. ^{[7
]}

Guillot, S. ^{[8
,9
]}

Harding, A. K. ^{[10
]}

Ho, W. C. G. ^{[11
,12
,13
]}

Lattimer, J. M. ^{[14
]}

Ludlam, R. M. ^{[15
]}

Mahmoodifar, S. ^{[1
,2
,10
]}

Morsink, S. M. ^{[16
]}

Ray, P. S. ^{[17
]}

Strohmayer, T. E. ^{[18
,19
]}

Wood, K. S. ^{[20
]}

Enoto, T. ^{[21
,22
]}

Foster, R. ^{[23
]}

Okajima, T. ^{[7
]}

Prigozhin, G. ^{[23
]}

Soong, Y. ^{[7
]}

机构：

[1] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[2] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA

[3] Univ Illinois, Ctr Theoret Astrophys, 1110 West Green St, Urbana, IL 61801 USA

[4] Univ Illinois, Dept Phys, 1110 West Green St, Urbana, IL 61801 USA

[5] Univ Illinois, Dept Astron, 1002 West Green St, Urbana, IL 61801 USA

[6] Columbia Univ, Columbia Astrophys Lab, 550 West 120th St, New York, NY 10027 USA

[7] NASA, Xray Astrophys Lab, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA

[8] CNRS, IRAP, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France

[9] Univ Toulouse, CNES, UPS, OMP, F-31028 Toulouse, France

[10] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[11] Haverford Coll, Dept Phys & Astron, 370 Lancaster Ave, Haverford, PA 19041 USA

[12] Univ Southampton, Math Sci Phys & Astron, Southampton SO17 1BJ, Hants, England

[13] Univ Southampton, STAG Res Ctr, Southampton SO17 1BJ, Hants, England

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

[15] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA

[16] Univ Alberta, Dept Phys, 4-183 CCIS, Edmonton, AB T6G 2E1, Canada

[17] US Naval Res Lab, Space Sci Div, Washington, DC 20375 USA

[18] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA

[19] NASA, Goddard Space Flight Ctr, Joint Space Sci Inst, Greenbelt, MD 20771 USA

[20] US Naval Res Lab, Washington, DC 20375 USA

[21] Kyoto Univ, Hakubi Ctr Adv Res, Kyoto 6068302, Japan

[22] Kyoto Univ, Dept Astron, Kyoto 6068302, Japan

[23] MIT, MIT Kavli Inst Astrophys & Space Res, 70 Vassar St, Cambridge, MA 02139 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2019年 / 887卷 / 01期

基金：

美国国家科学基金会;

关键词：

EQUATION-OF-STATE; X-RAY-EMISSION; DENSE MATTER; MILLISECOND PULSARS; PAIR CREATION; LIGHT CURVES; POLAR CAPS; ATMOSPHERES; EVOLUTION; VIEW;

D O I：

10.3847/2041-8213/ab50c5

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Neutron stars are not only of astrophysical interest, but are also of great interest to nuclear physicists because their attributes can be used to determine the properties of the dense matter in their cores. One of the most informative approaches for determining the equation of state (EoS) of this dense matter is to measure both a star's equatorial circumferential radius R-e and its gravitational mass M. Here we report estimates of the mass and radius of the isolated 205.53 Hz millisecond pulsar PSR J0030+0451 obtained using a Bayesian inference approach to analyze its energy-dependent thermal X-ray waveform, which was observed using the Neutron Star Interior Composition Explorer (NICER). This approach is thought to be less subject to systematic errors than other approaches for estimating neutron star radii. We explored a variety of emission patterns on the stellar surface. Our best-fit model has three oval, uniform-temperature emitting spots and provides an excellent description of the pulse waveform observed using NICER. The radius and mass estimates given by this model are R-e = 13.02(-1.06)(+1.24) km and M = 1.44(-0.14)(+0.15) M-circle dot (68%). The independent analysis reported in the companion paper by Riley et al. explores different emitting spot models, but finds spot shapes and locations and estimates of R-e and M that are consistent with those found in this work. We show that our measurements of R-e and M for PSR J0030+0451 improve the astrophysical constraints on the EoS of cold, catalyzed matter above nuclear saturation density.

引用

页数：28

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