Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 1975
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975nyasa.262..404h&link_type=abstract
(AAS, American Physical Society, and New York Academy of Sciences, Texas Symposium on Relativistic Astrophysics, 7th, Dallas, Te
Astronomy and Astrophysics
Astronomy
Black Holes (Astronomy), Density (Mass/Volume), Neutron Stars, Stellar Mass, Astronomical Models, Compressibility Effects, Critical Mass, Gravitational Collapse, Stellar Envelopes
Scientific paper
The maximum mass of a nonrotating neutron star is calculated. A dimensional argument is used to show that the mass of a star is affected by two physical variables, the compressibility and density of its matter. By application of the general relativistic equations of hydrostatic equilibrium to incompressible matter, the dependence of mass on a limiting equation of state is eliminated. The mass is determined by selection of a maximum permissible density. The calculation is based on a model consisting of an outer envelope of realistic neutron matter extending inward to a critical density beyond which matter is considered to be incompressible and above which current neutron matter calculations are unreliable. The core is stable against radial oscillations; pressure is assumed to be only a function of density. The core density is considered to have the maximum value for which the pressure may be accurately calculated from nuclear theory. The surface pressure boundary for the core, which must be matched by the exterior mass shell, is determined from this value. The maximum core mass is determined to be 7.95 solar masses, corresponding to an envelope mass of 0.01 solar masses.
Cohen Jeffery M.
Hegyi Dennis J.
Lee Tsung-Shung H.
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