GW170817: Joint Constraint on the Neutron Star Equation of State from Multimessenger Observations
نویسندگان
چکیده
منابع مشابه
Constraints on the Equation of State of Neutron Star Matter From Observations of Kilohertz QPOs
The frequencies of the highest-frequency kilohertz QPOs recently discovered in some sixteen neutron stars in low-mass X-ray binary systems are most likely the orbital frequencies of gas in Keplerian orbit around these neutron stars. If so, these QPOs provide tight upper bounds on the masses and radii of these neutron stars and important new constraints on the equation of state of neutron star m...
متن کاملOn the Progenitor of Binary Neutron Star Merger GW170817
On 2017 August 17 the merger of two compact objects with masses consistent with two neutron stars was discovered through gravitational-wave (GW170817), gamma-ray (GRB170817A), and optical (SSS17a/AT 2017gfo) observations. The optical source was associated with the early-type galaxy NGC 4993 at a distance of just ∼40 Mpc, consistent with the gravitational-wave measurement, and the merger was lo...
متن کاملOn the Progenitor of Binary Neutron Star Merger Gw170817
On August 17, 2017 the merger of two compact objects with masses consistent with two neutron stars was discovered through gravitational-wave (GW170817), gamma-ray (GRB170817A), and optical (SSS17a/AT 2017gfo) observations. The optical source was associated with the early-type galaxy NGC 4993 at a distance of just ∼40 Mpc, consistent with the gravitationalwave measurement, and the merger was loc...
متن کاملPulsar Constraints on Neutron Star Structure and Equation of State
The sudden spin jumps, or glitches, commonly seen in isolated neutron stars are thought to represent angular momentum transfer between the crust and the liquid interior [1]. In this picture, as a neutron star’s crust spins down under magnetic torque, differential rotation develops between the stellar crust and a portion of the liquid interior. The more rapidly rotating component then acts as an...
متن کاملNeutron Star Structure and the Equation of State
The structure of neutron stars is considered from theoretical and observational perspectives. We demonstrate an important aspect of neutron star structure: the neutron star radius is primarily determined by the behavior of the pressure of matter in the vicinity of nuclear matter equilibrium density. In the event that extreme softening does not occur at these densities, the radius is virtually i...
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ژورنال
عنوان ژورنال: The Astrophysical Journal
سال: 2018
ISSN: 2041-8213
DOI: 10.3847/2041-8213/aaa402