Uncertainty in the saturation density of nuclear matter and neutron star models

Details Uncertainty in the saturation density of nuclear matter and neutron star models Uncertainty in the saturation density of nuclear matter and neutron star models

Oct 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a...102..299h&link_type=abstract

Astronomy and Astrophysics, vol. 102, no. 3, Oct. 1981, p. 299-302. Research supported by the U.S. - Maria Sklodowska-Curie Fun

Astronomy and Astrophysics

Astrophysics

23

Neutron Stars, Nuclear Particles, Particle Density (Concentration), Stellar Mass, Stellar Models, Equations Of State, Field Theory (Physics), Matter (Physics), Nuclear Astrophysics, Nucleons

Scientific paper

A study of consequences of uncertainties in values ascribed to atomic nuclei on neutron star models is presented. The discussion is limited to the relativistic mean field theory of dense matter, with the interaction of nucleons described by the exchange of neutral scalar and neutral vector mesons, pions, and rho mesons. Coupling constants are determined by fitting the experimental saturation properties of nuclear matter, for which uncertainties imply uncertainties in the equation of state of dense matter, and thereby neutron star models. An empirical value is assumed for the saturation density of nuclear matter, obtained from a Hartree-Fock approximation, and values of the gravitational mass, stellar radius, total number of baryons, and the moment of inertia of neutron stars are calculated. Finally, it is noted that the relativistic mean field theory will be quantitatively correct only in regions of sufficient baryon density.

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