Analytic relativistic model for a superdense star

Details Analytic relativistic model for a superdense star Analytic relativistic model for a superdense star

Jul 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985gregr..17..671d&link_type=abstract

General Relativity and Gravitation (ISSN 0001-7701), vol. 17, July 1985, p. 671-681.

Physics

21

Neutron Stars, Relativistic Theory, Stellar Mass, Stellar Models, Supermassive Stars, Analytic Functions, Density Distribution, Einstein Equations, Gravitational Fields, Red Shift, Stellar Structure, Systems Stability

Scientific paper

A new analytic relativistic model has been obtained for superdense stars by solving the Einstein field equations for the spherically symmetric and static case. The model stands all the tests of physical reality. The density (rho) remains positive under all conditions and decreases smoothly from the center to the surface of the structure. The pressure (P), the ratio P/rho and dP/d(rho) and dP/d(rho) decrease with decreasing density. For all the finite values of pressure, the configurations are stable under radial perturbation. For dP/d(rho) less than or equal to 1, the maximum mass of neutron star model is 4.17 solar mass, and the surface and central redshifts are 0.63 and 1.60, respectively. For an infinite central pressure, the surface redshift is 1.61. The structures are bound, and the binding coefficients increase with the increasing mass.

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