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Neutron Star Mass and Radius Measurements

Department of Physics & Astronomy, Stony Brook University, Stony Brook, NY 11794-3800, USA
Universe 2019, 5(7), 159; https://doi.org/10.3390/universe5070159
Received: 24 May 2019 / Revised: 19 June 2019 / Accepted: 21 June 2019 / Published: 28 June 2019
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Abstract

Constraints on neutron star masses and radii now come from a variety of sources: theoretical and experimental nuclear physics, astrophysical observations including pulsar timing, thermal and bursting X-ray sources, and gravitational waves, and the assumptions inherent to general relativity and causality of the equation of state. These measurements and assumptions also result in restrictions on the dense matter equation of state. The two most important structural parameters of neutron stars are their typical radii, which impacts intermediate densities in the range of one to two times the nuclear saturation density, and the maximum mass, which impacts the densities beyond about three times the saturation density. Especially intriguing has been the multi-messenger event GW170817, the first observed binary neutron star merger, which provided direct estimates of both stellar masses and radii as well as an upper bound to the maximum mass. View Full-Text
Keywords: neutron stars; dense matter equation of state; nuclear structure; gravitational waves neutron stars; dense matter equation of state; nuclear structure; gravitational waves
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Lattimer, J.M. Neutron Star Mass and Radius Measurements. Universe 2019, 5, 159.

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