2009
DOI: 10.1088/0004-637x/693/2/1775
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The Mass and Radius of the Neutron Star in Exo 1745–248

Abstract: Bursting X-ray binaries in globular clusters are ideal sources for measuring neutron star masses and radii, and hence, for determining the equation of state of cold, ultradense matter. We use time-resolved spectroscopic data from EXO 1745−248 during thermonuclear bursts that show strong evidence for photospheric radius expansion to measure the Eddington flux and the apparent surface area of the neutron star. We combine this with the recent measurement of the distance to the globular cluster Terzan 5, where thi… Show more

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Cited by 273 publications
(194 citation statements)
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“…[23] (Ref. [24]), based on six (eight) neutron star observations of the X-ray bursts [16][17][18][19] and thermal emissions from quiescent low-mass X-ray binaries (LMXBs) in the globular clusters [20][21][22].…”
Section: Numerical Results and Discussionmentioning
confidence: 99%
See 1 more Smart Citation
“…[23] (Ref. [24]), based on six (eight) neutron star observations of the X-ray bursts [16][17][18][19] and thermal emissions from quiescent low-mass X-ray binaries (LMXBs) in the globular clusters [20][21][22].…”
Section: Numerical Results and Discussionmentioning
confidence: 99%
“…Interestingly, more and more neutron star observations, especially, the accurate measurement of the pulsar J1614-2230 with the mass 1.97 ± 0.04 M ⊙ [15], the astrophysical observations of X-ray bursts [16][17][18][19] and thermal emissions from quiescent low-mass X-ray binaries (LMXBs) in the globular clusters [20][21][22], gradually provide a reliable constraint on the mass-radius relations which is tightly connected to the EoS of neutron star matter. The analysis of these astrophysical observations shows that the radius of a 1.4 solar mass neutron star lies between 10.4 and 12.9 km, independent of assumptions about the composition of the core [23,24].…”
Section: Introductionmentioning
confidence: 99%
“…The Eddington fluxes, measured in bright bursts that show photospheric radius expansion, have a different dependence on mass and radius, as shown in Equation (37). The combination of these measurements, together with an estimate of the distance to each source, has led to the determination of the neutron star radii in a number of bursters to date, with weakly correlated errors (Özel, Güver, & Psaltis 2009;Güver et al 2010a;Güver et al 2010b;Özel, Gould, & Güver 2012). The results for 4U 1608−52, KS 1731-260, EXO 1745−248, and 4U 1820-30 are shown in Figure 11.…”
Section: Spectral Measurementsmentioning
confidence: 99%
“…The maximum stable neutron star mass can place constraints on the equation of state and the behavior of matter at nuclear densities (Glendenning & Schaffner-Bielich 1998;Lattimer & Prakash 2004Lackey et al 2006;Schulze et al 2006;Kurkela et al 2010; see also Demorest et al 2010 for recent observational results). Coupled mass/radius observations can place even stronger constraints on the the equation of state for dense matter (Özel et al 2009Steiner et al 2010Steiner et al , 2013Miller 2013). While X-ray bursts (XRBs) on neutron stars (van Paradijs 1979;van Paradijs & Lewin 1986;Ebisuzaki 1987;Damen et al 1990;van Paradijs et al 1990;Madej et al 2004;Majczyna et al 2005;Suleimanov et al 2011aSuleimanov et al , 2011bSuleimanov et al , 2012Miller et al 2011;Galloway & Lampe 2012;Poutanen et al 2014;Nättilä et al 2015;Kajava et al 2016), and thermal emission from quiescent and isolated neutron stars (Rutledge et al 1999;Heinke et al 2006;Ho et al 2007;Ho & Heinke 2009;Cackett et al 2010;Catuneanu et al 2013;Guillot et al 2013;Klochkov et al 2015;Ofengeim et al 2015) remain the most-studied observational probes providing simultaneous measurements of mass and radius, a growing list of observations have been proposed to provide this coupled data, from pulsar timing to gravitational wave signals from merging neutron stars (for a review, see Lattimer 2012).…”
Section: Introductionmentioning
confidence: 99%
“…Two of the largest uncertainties are in the distances to the XRB sources and their atmospheric compositions (e.g., Strohmayer & Bildsten 2006;Lattimer & Steiner 2014). There are also uncertainties in how the physics of the burst correlates with the observations, for example, at what times during an observation the photosphere is expanding, contracting, or has reached "touchdown"; i.e., at what time the photosphere has returned to (approximately) its pre-burst radius (see Özel et al 2009;Steiner et al 2010). Finally, there are uncertainties in the model approximations and techniques, which lead to discrepancies in the results of different modeling groups.…”
Section: Introductionmentioning
confidence: 99%