A two-solar-mass neutron star measured using Shapiro delay

By P. Demorest, T. Pennucci, S. Ransom, M. Roberts, Jason W. T. Hessels. Nature, 2010

2,309 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/69c95754b0ee30ca0631db1ff00637b10a08edae

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Citations in the corpus

CORE-COLLAPSE SUPERNOVA EXPLOSIONS TRIGGERED BY A QUARK–HADRON PHASE TRANSITION DURING THE EARLY POST-BOUNCE PHASE (2010, background): “The recent mass measurement by Demorest et al. (2010) points to an even higher neutron star mass of 1.97 ± 0.04 M⊙.”
PULSAR J0453+1559: A DOUBLE NEUTRON STAR SYSTEM WITH A LARGE MASS ASYMMETRY (2015, background): “However, from an analysis of the evolution of PSR J1614–2230, Tauris et al. (2011) had already suggested that at least some NSs must be born more massive than 1.44 Me.”
NEUTRON STAR MASSES AND RADII FROM QUIESCENT LOW-MASS X-RAY BINARIES (2013, background): “…of sound to be less than the speed of light), general relativity and observations (i.e., restricting the minimum maximum neutron star mass (M̂) to be larger than M̂ = 1.93 M⊙, the 1σ lower limit to the mass of pulsar PSR J1614-2230 (Demorest et al. 2010), the most massive precision measurement.”
r-PROCESS NUCLEOSYNTHESIS IN DYNAMICALLY EJECTED MATTER OF NEUTRON STAR MERGERS (2011, result): “…the EOS influence on gross properties of the ejecta, we also performed simulations with the Lattimer et al. (1991) LS220 EOS with an incompressibility modulus of 220 MeV and a NS radius of ∼12 km. Note that both of our EOSs are in agreement with the observation of a 2M NS (Demorest et al. 2010).”
The electromagnetic signals of compact binary mergers (2012, background): “PSR J1614−2230 with a mass of 1.97 ± 0.04 M (Demorest et al. 2010) is nowadays considered as a robust lower limit on the maximum ns mass, but even ns with considerably larger masses are not implausible.”
CORE-COLLAPSE SUPERNOVA EQUATIONS OF STATE BASED ON NEUTRON STAR OBSERVATIONS (2012, background): “…with those inferred from experiment, (ii) maximum neutron star masses large enough to be consistent with the recent measurement of a 1.97 solar mass neutron star in Demorest et al. (2010), and (iii) masses and radii consistent with recent neutron star observations of e.g. Steiner et al. (2010).”
Approximate Universal Relations for Neutron Stars and Quark Stars (2016, background): “Observe how the mass-radius curve can be drastically different as one varies the equation of state, with most still passing the constraints imposed by the massive pulsars J1614-2230 [122, 138] (green dot-dashed horizontal line), J0348+0432 [123] (red dot-dashed horizontal line) and Vela X-1 [124–126”
Optical and X-ray emission from stable millisecond magnetars formed from the merger of binary neutron stars (2013, result): “The recent discovery of massive∼ 2M⊙ NSs (Demorest et al. 2010; Antoniadis et al. 2013) indicates that the EoS is not as soft as predicted by some previous models.”
THE SECOND FERMI LARGE AREA TELESCOPE CATALOG OF GAMMA-RAY PULSARS (2013, neutral): “; (3) Ransom et al. (2011); (4) This paper; (5) Demorest et al. (2010); (6) Kerr et al. (2012b); (7) Guillemot et al. (2012).”
Red or blue? A potential kilonova imprint of the delay until black hole formation following a neutron star merger (2014, background): “Our approximation is justified in that HMNSs from self-consistent calculations achieve a state of quasi-equilibrium over a few dynamical times after the merger, particularly if they are not too close to the mass for prompt BH formation (e.g. Sekiguchi et al. 2011).”
The Masses and Spins of Neutron Stars and Stellar-Mass Black Holes (2014, background): “The first of these, PSR J1614−2230 [112], is a pulsar-white dwarf system that had its Shapiro delay measured due to its fortunate nearly edge-on orientation.”
AN OPEN-SOURCE NEUTRINO RADIATION HYDRODYNAMICS CODE FOR CORE-COLLAPSE SUPERNOVAE (2014, methodology): “This maximum mass has been ruled out by the observation of ∼2 M neutron stars (Demorest et al. 2010; Antoniadis et al. 2013), however, it has been used in several other studies as a basis for comparison (Liebendörfer et al. 2005; Müller et al. 2010).”
Formation of Double Neutron Star Systems (2017, background): “…equation-of-state (EoS) of nuclear matter at high densities (Lattimer & Prakash 2007; Kehl et al. 2016; Özel & Freire 2016), although tighter constraints have so far been obtained from massive NSs with an orbiting white dwarf (WD) companion (Demorest et al. 2010; Antoniadis et al. 2013).”