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Observational constraints on neutron star masses and radii

  • M. Coleman MillerEmail author
  • Frederick K. Lamb
Regular Article - Theoretical Physics
Part of the following topical collections:
  1. Exotic Matter in Neutron Stars

Abstract.

Precise and reliable measurements of the masses and radii of neutron stars with a variety of masses would provide valuable guidance for improving models of the properties of cold matter with densities above the saturation density of nuclear matter. Several different approaches for measuring the masses and radii of neutron stars have been tried or proposed, including analyzing the X-ray fluxes and spectra of the emission from neutron stars in quiescent low-mass X-ray binary systems and thermonuclear burst sources; fitting the energy-dependent X-ray waveforms of rotation-powered millisecond pulsars, burst oscillations with millisecond periods, and accretion-powered millisecond pulsars; and modeling the gravitational radiation waveforms of coalescing double neutron star and neutron star - black hole binary systems. We describe the strengths and weaknesses of these approaches, most of which currently have substantial systematic errors, and discuss the prospects for decreasing the systematic errors in each method.

Keywords

Neutron Star Stellar Surface Burst Data Posterior Probability Density Planck Function 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© SIF, Springer-Verlag Berlin Heidelberg 2016

Authors and Affiliations

  1. 1.Department of Astronomy and Joint Space-Science InstituteUniversity of MarylandCollege ParkUSA
  2. 2.Center for Theoretical Astrophysics and Department of PhysicsUniversity of Illinois at Urbana-ChampaignUrbanaUSA
  3. 3.Department of AstronomyUniversity of Illinois at Urbana-ChampaignUrbanaUSA

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