Determining the nuclear equation of state from neutron-star masses and radii

Details Determining the nuclear equation of state from neutron-star masses and radii Determining the nuclear equation of state from neutron-star masses and radii

Oct 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...398..569l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 398, no. 2, p. 569-573.

Statistics

Computation

66

Equations Of State, Neutron Stars, Nuclear Astrophysics, Stellar Mass, Barotropism, Computational Astrophysics, Radii, Stellar Interiors, Stellar Physics

Scientific paper

A method is developed for determining the nuclear equation of state directly from a knowledge of the masses and radii of neutron stars. This analysis assumes only that equilibrium neutron-star matter has the stress-energy tensor of an isotropic fluid with a barotropic equation of state, and that general relativity describes a neutron star's internal gravitational field. We present numerical examples which illustrate how well this method will determine the equation of state when the appropriate observational data become available.

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