The radius of the quiescent neutron star in the globular cluster M13

Shaw, A. W.; Heinke, C. O.; Steiner, A. W.; Campana, S.; Cohn, H. N.; Ho, W. C. G.; Lugger, P. M.; Servillat, M.

doi:10.1093/mnras/sty582

Title: The radius of the quiescent neutron star in the globular cluster M13

Journal Article · Tue Mar 06 00:00:00 EST 2018 · Monthly Notices of the Royal Astronomical Society

DOI:https://doi.org/10.1093/mnras/sty582· OSTI ID:1460182

Shaw, A. W. ^[1]; Heinke, C. O. ^[1]; Steiner, A. W. ^[2]; Campana, S. ^[3]; Cohn, H. N. ^[4];

^[5]; Lugger, P. M. ^[4]; Servillat, M. ^[6]

Univ. of Alberta, Edmonton, AB (Canada). Dept. of Physics
Univ. of Tennessee, Knoxville, TN (United States). Dept. of Physics and Astronomy; Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Physics Division
INAF Brera Astronomical Observatory, Milan (Italy)
Indiana Univ., Bloomington, IN (United States). Dept. of Astronomy
Haverford College, PA (United States). Dept. of Physics and Astronomy; Univ. of Southampton (United Kingdom). Mathematical Sciences, Physics & Astronomy. STAG Research Centre
Paris Diderot Univ., Meudon (France). PSL Research Univ. Paris Observatory. Lab. for the Universe and Theory (LUTH)

X-ray spectra of quiescent low-mass X-ray binaries containing neutron stars can be fit with atmosphere models to constrain the mass and the radius. Mass-radius constraints can be used to place limits on the equation of state of dense matter. In this paper, we perform fits to the X-ray spectrum of a quiescent neutron star in the globular cluster M13, utilizing data from ROSAT, Chandra, and XMM–Newton, and constrain the mass–radius relation. Assuming an atmosphere composed of hydrogen and a 1.4 M_⊙ neutron star, we find the radius to be R_NS = 12.2^+1.5_-1.1 km, a significant improvement in precision over previous measurements. Incorporating an uncertainty on the distance to M13 relaxes the radius constraints slightly and we find R_NS = 12.3^+1.9_-1.7 km (for a 1.4M_⊙ neutron star with a hydrogen atmosphere), which is still an improvement in precision over previous measurements, some of which do not consider distance uncertainty. Finally, we also discuss how the composition of the atmosphere affects the derived radius, finding that a helium atmosphere implies a significantly larger radius.

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Research Organization:: Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States); Univ. of Tennessee, Knoxville, TN (United States); Univ. of Alberta, Edmonton, AB (Canada); Univ. of Southampton (United Kingdom)

Sponsoring Organization:: USDOE; National Science Foundation (NSF); Natural Sciences and Engineering Research Council of Canada (NSERC); Science and Technology Facilities Council (STFC) (United Kingdom)

Grant/Contract Number:: AC05-00OR22725; PHY1554876; ST/M000931/1

OSTI ID:: 1460182

Journal Information:: Monthly Notices of the Royal Astronomical Society, Vol. 476, Issue 4; ISSN 0035-8711

Publisher:: Royal Astronomical SocietyCopyright Statement

Country of Publication:: United States

Language:: English

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Cited by: 19 works

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