Equation of state constraints from neutron stars

Conference paper

Abstract

Recent measurements of thermal radiation from neutron stars have suggested a rather broad range of radiation radii ( \(R_{\infty}=R/\sqrt{1-2GM/Rc^{2}}\,\) ). Sources in M13 and Omega Cen imply R ∞∼12–14 km, but X7 in 47 Tuc implies R ∞∼16–20 km and RX J1856-3754 R ∞>17 km. If these measurements are all correct, only a limited selection of EOS’s could be consistent with them, but a broad range of neutron star masses (up to 2 M⊙) would also be necessary. The surviving equations of state are incompatible with significant softening above nuclear saturation densities, such as would occur with Boson condensates, a low-density quark-hadron transition, or hyperons. Other potential constraints, such as from QPO’s, radio pulsar mass and moment of inertia measurements, and neutron star cooling, are compared.

Keywords

Neutron stars Equation of state Pulsars 

PACS

26.60.+c 97.60.Jd 7.60.Gb 
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Copyright information

© Springer 2007

Authors and Affiliations

  1. 1.Department of Physics and AstronomyStony Brook UniversityStony BrookUSA

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