Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995ap%26ss.225....1p&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 225, no. 1, p. 1-16
Astronomy and Astrophysics
Astrophysics
Density (Mass/Volume), Neutron Stars, Radii, Stellar Composition, Stellar Interiors, Charge Distribution, Energy Distribution, Mass Distribution, Pressure Distribution
Scientific paper
With the assumption, the physical 3-space t = constant in a superdense star is spheroidal and the matter-density on the boundary surface of the configuration rhoa = 2 x 1014 g/cu cm (approximately the average matter density in a neutron star) Vaidya and Tikekar (1982) proposed an exact relativistic model for a neutron star. They suggested that their model can describe the hydrostatic equilibrium conditions in such a superdense star with densities in the range of 1014 - 1016 g/cu cm. Based on this model Parui and Sarma (1991) estimated the maximum limit of the density variation parameter lambda for a stable neutron star (both for charged and uncharged) which is equal to 0.68, i.e. lambdamax = 0.68. In this paper we have shown variation of central density per unit equilibrium radius (rho0/a), variation of mass, upper limit of density variation parameter lambda both for charged and uncharged neutron stars at densities 1015 and 1016 g/cu cm, respectively. We have obtained lambdamax = 0.68, i.e. the same as before. The important is that the duration of stability among the neutron star's constituents around lambdamax will be shorter and shorter at higher densities as we proceed near the center of the neutron star. In case of a charged neutron star, once stability among the constituents has been established, then unstability appears gradually maintaining linear relation between change in central density per unit equilibrium radius and change in mass whereas in case of uncharged neutron star, linear relation does not maintain.
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