Astrophysical measurement of the equation of state of neutron star matter

By F. Özel, G. Baym, T. Guver. 2010

223 citations recorded by the source corpus.

We present the first astrophysical measurement of the pressure of cold matter above nuclear saturation density, based on recently determined masses and radii of three neutron stars. The pressure at higher densities is below the predictions of equations of state that account only for nucleonic degrees of freedom, and thus present a challenge to the microscopic theory of neutron star matter.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/bc8d3f6d5d79066e779de82302a87ac039fb1a7d

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In Astronomy and Astrophysics

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

Citations in the corpus

• Strongly correlated quantum fluids: ultracold quantum gases, quantum chromodynamic plasmas and holographic duality (2012, background): “There is a very active program to pin down this relationship using observations of compact stars [445, 446].”
• THE DENSE MATTER EQUATION OF STATE FROM NEUTRON STAR RADIUS AND MASS MEASUREMENTS (2015, methodology): “Özel et al. (2010) used one of these mapping techniques on the radius measurements obtained from thermonuclear bursters to place the first constraints on the neutron star equation of state at high densities.”
• Constraining the mass and radius of neutron stars in globular clusters (2017, methodology): “From the eight probability distributions for each neutron star, we can directly apply a generalization of the approach first described in Özel & Psaltis (2009), Steiner et al. (2010), and Özel et al. (2010).”
• Constraints on perturbative f(R) gravity via neutron stars (2010, methodology): “After the tight constraints obtained in [38], it seems this is no longer quite true.”
• Signatures of magnetar central engines in short GRB light curves (2013, background): “Ozel et al. (2010b) show that, for a maximum nonrotating NS mass ofMmax =2.1 M⊙, the merger of two NSs with a total mass6 1.4Mmax will have a delayed collapse to a BH (i.e. a magnetar phase).”
• 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).”
• Evidence for a maximum mass cut-off in the neutron star mass distribution and constraints on the equation of state (2017, background): “Measurements of NS masses and radii together can put strong constraints on the EoS (Read et al. 2009; Özel & Psaltis 2009; Özel et al. 2010; Steiner et al. 2010; Guillot et al. 2013; Steiner et al. 2013a,b; Özel et al. 2016).”
• The phase diagram of dense QCD (2010, background): “Besides, recent attempts to determine the mass and the radius of neutron stars from X-ray bursts would be an alternative way to access the equation of state of dense QCD [263, 264].”