Neutron Star Observations and the Equation of State

Journal Article · Thu May 07 00:00:00 EDT 2009 · AIP Conference Proceedings

DOI:https://doi.org/10.1063/1.3146211· OSTI ID:21304906

Lattimer, James M ^[1]

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1. Department of Physics and Astronomy, Stony Brook University, Stony Brook, NY 11794-3800 (United States)

This talk reviews limits to the properties of neutron stars established from physical considerations such as causality and stability. In addition, it summarizes recent attempts to determine realistic bounds to the equation of state (EOS) from a simultaneous measurement of a neutron star's mass and radius. Observational constraints on the neutron star radius from thermal emission, seismology, spin-orbit coupling, and tidal effects in mergers are discussed. Possible constraints from neutron star cooling, including neutrino emissions, are discussed.

• OSTI ID: 21304906
• Journal Information: AIP Conference Proceedings, Vol. 1128, Issue 1; Conference: 5. ANL/MSU/JINA/INT FRIB workshop on bulk nuclear properties, East Lansing, MI (United States), 19-22 Nov 2008; Other Information: DOI: 10.1063/1.3146211; (c) 2009 American Institute of Physics; Country of input: International Atomic Energy Agency (IAEA); ISSN 0094-243X
• Country of Publication: United States
• Language: English

Related Subjects

73 NUCLEAR PHYSICS AND RADIATION PHYSICS
CAUSALITY
EQUATIONS OF STATE
L-S COUPLING
NEUTRINOS
NEUTRON STARS
NUCLEAR MATTER
SPIN
STABILITY