Shapiro delay measurement of a two solar mass neutron star

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

1,099 citations recorded by the source corpus.

Neutron stars are composed of the densest form of matter known to exist in our universe, and thus provide a unique laboratory for exploring the properties of cold matter at supranuclear density. Measurements of the masses or radii of these objects can strongly constrain the neutron-star matter equation of state, and consequently the interior composition of neutron stars[1, 2]. Neutron stars that are visible as millisecond radio pulsars are especially useful in this respect, as timing observations of the radio pulses provide an extremely precise probe of both the pulsar’s motion and the surrounding space-time metric. In particular, for a pulsar in a binary system, detection of the general relativistic Shapiro delay allows us to infer the masses of both the neutron star and its binary

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

View Paper: https://www.semanticscholar.org/paper/3c175b91685ab6b3cca3a9cc27f1e04c996a0381

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Citations in the corpus

Generic conditions for stable hybrid stars (2013, methodology): “Using the CSS parameterization (1) of the quark matter EoS, it is possible to get hybrid stars that are heavy enough to be consistent with recent measurements of stars of mass 2M [41, 42].”
Antinuclei in heavy-ion collisions (2018, background): “This makes it extremely difficult to describe recent observations [210, 211] of neutron stars with masses above twice the solar mass.”
Stellar structure models in modified theories of gravity: Lessons and challenges (2019, methodology): “80M⊙ [16, 78]); the SLy model of effective nuclear hamiltonian obtained from many-body calculations with a simple two-nucleon potential and a modelling of the crust-core transitions as a weak first-order transition with a minor density jump [189, 190, 191, 192], which typically admits analytical rep”
Unequal mass binary neutron star mergers and multimessenger signals (2016, result): “All three EoS are consistent with neutron stars having a mass of at least 2M , and they are therefore consistent with observations of NS masses [30, 31].”
The NANOGrav 15 yr Data Set: Observations and Timing of 68 Millisecond Pulsars (2023, background): “Relative to the recent, larger uncertainty, the value of Pb increased by 4.3σ. Newly measured RN in PSR J1614−2230 (one of the highest-mass neutron stars known; see Demorest et al. 2010) was accompanied by a 3.8σ increase in Pb.”
Constraints on perturbative f(R) gravity via neutron stars (2010, background): “Apart from the above constraint, the recent measurement [41] of the mass of the neutron star PSR J1614-2230 with 1.”
Hyperons in neutron star matter within relativistic mean-field models (2014, background): “However, in the standard picture, the opening of hyperon degrees of freedom leads to a considerable softening of the EoS [1], which in turns leads to maximum neutron star masses smaller than the highest observed values [2].”