THE MASS AND RADIUS OF THE NEUTRON STAR IN 4U 1820−30

By T. Güver, P. Wroblewski, L. Camarota, F. Özel. 2010

193 citations recorded by the source corpus.

We report on the measurement of the mass and radius of the neutron star in the low-mass X-ray binary 4U 1820−30. The analysis of the spectroscopic data on multiple thermonuclear bursts yields well-constrained values for the apparent emitting area and the Eddington flux, both of which depend in a distinct way on the mass and radius of the neutron star. The distance to the source is that of the globular cluster NGC 6624, where the source resides. Combining these measurements, we uniquely determine the probability density over the stellar mass and radius. We find the mass to be M = 1.58 ± 0.06 M☉ and the radius to be R = 9.1 ± 0.4 km.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/0fea167bf92c29a4374d547acc1fc262360747c5

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In Astronomy and Astrophysics

1. J. Lattimer
2. A. Steiner
3. S. Guillot
4. C. Heinke
5. F. Özel
6. T. Güver
7. Dimitrios Psaltis
8. G. Baym

Citations in the corpus

• ON THE MASS DISTRIBUTION AND BIRTH MASSES OF NEUTRON STARS (2012, unknown): “This category includes 4U 1745−248 (Özel et al. 2009), 4U 1608−52 (Güver et al. 2010a), 4U 1820−30 (Güver et al. 2010b), and KS 1731−260 (Özel et al. 2012).”
• Constraints on perturbative f(R) gravity via neutron stars (2010, methodology): “These data are provided by the measurements on the neutron stars EXO 1745-248 [44], 4U 1608-52 [45] and 4U 1820-30 [46] by the methods described in the cited papers.”
• Constraining the mass and radius of neutron stars in globular clusters (2017, background): “Steiner et al. (2010) combined mass-radius constraints from three thermonuclear burst systems (Özel et al. 2009; Güver et al. 2010a,b) with results from three quiescent LMXBs (Heinke et al. 2006b; Webb & Barret 2007).”
• THE EQUATION OF STATE FROM OBSERVED MASSES AND RADII OF NEUTRON STARS (2010, methodology): “Touchdown flux: Five of the bursts have a measured touchdown flux:FTD,∞/(10−8 ergs cm−2 s−2) = 5.33±0.27, 5.65±0.20, 5.12±0.15, 5.24±0.19, and 5.42±0.16 (Güver et al. 2010b).”
• Strange star equation of state fits the refined mass measurement of 12 pulsars and predicts their radii (2013, background): “In a recent work, Güver et al. (2010a) used time resolved X-ray Downloaded from https://academic.oup.com/mnras/article-abstract/431/4/3216/1142246 by guest on 29 July 2018 spectroscopy of the thermonuclear burst of 4U 1820−30, and side by side they measured the distance of the globular cluster NGC…”
• NEUTRON STAR MASSES AND RADII FROM QUIESCENT LOW-MASS X-RAY BINARIES (2013, methodology): “In addition, they have been largely modeled (Özel, Güver & Psaltis 2009; Güver et al. 2010a,b; Özel, Baym & Güver 2010; Steiner, Lattimer & Brown 2010; Özel, Gould & Güver 2012; Suleimanov, Poutanen & Werner 2011; Steiner, Lattimer & Brown 2013) with static atmospheres but are certainly…”
• THE DENSE MATTER EQUATION OF STATE FROM NEUTRON STAR RADIUS AND MASS MEASUREMENTS (2015, methodology): “Without any further information to choose between the optical and the near-IR measurements, Güver et al. (2010b) combined them into a single boxcar likelihood between 6.8 to 9.6 kpc, which placed more than warranted likelihoods at the shortest and intermediate distances.”
• MEASUREMENT OF THE RADIUS OF NEUTRON STARS WITH HIGH SIGNAL-TO-NOISE QUIESCENT LOW-MASS X-RAY BINARIES IN GLOBULAR CLUSTERS (2012, unknown): “The LMXBs EXO 1745-248, 4U 1608-52, and 4U 1820- 30 were found to have respective radii in the 2σ ranges RNS = [7.5 − 11.0] km (Özel et al. 2009), RNS = [7.5 − 11.5] km (Güver et al. 2010a) and RNS = [8.5 − 9.5] km (Güver et al. 2010b), respectively.”