Abstract
Exact solutions have been obtained for a massive fluid sphere under the extreme causality condition (dP/dρ)=1. Radial pulsational stability of these structures has been discussed. It is found that for pulsationally stable configurations the surface to central density ratio is greater than 0.30, the maximum values for surface and central redshifts are 0.85 and 3.40 respectively in the extreme case, and the maximum mass and size are respectively 4.8M ⊙ and 20.1 km. It has also been shown that these structures are gravitationally bound, with a maximum binding energy per unit rest mass equal to 0.25 for a surface to central density ratio ≃0.40. Slow rotation of these configurations has also been considered, and the relative drag and moment of inertia have been calculated. These results have been applied to the Crab pulsar and the mass of the pulsar has also been calculated based upon this model.
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References
Baldwin, J. E.: 1971, in R. D. Davies and F. G. Smith (eds.), ‘The Crab Nebula’,IAU Symp. 46, 226.
Bardeen, J. M., Thorne, K. S., and Meltzer, D. W.: 1966,Astrophys. J. 145, 505.
Baym, G., Pethick, C. J., and Sutherland, P.: 1971,Astrophys. J. 170, 299.
Bethe, H. A., Borner, G., and Sato, K.: 1971,Astron. Astrophys. 7, 279.
Bethe, H. A.: 1974, in C. J. Hansen (ed.), ‘Physics of Dense Matter’,IAU Symp. 53, 27.
Bondi, H.: 1964,Proc. Roy. Soc. A282, 303.
Borner, G.: 1973,Springer Tracts in Modern Physics, Vol. 69.
Brecher, K. and Caporosso, G.: 1976,Nature 259, 377.
Cameron, A. G. W.: 1969,Astrophys. Space Sci. 5, 113.
Chandrasekhar, S. and Miller, J. C.: 1974,Monthly Notices Roy. Astron. Soc. 167, 63.
Cohen, J. M. and Cameron, A. G. W.: 1971,Astrophys. Space Sci. 10, 227.
Cohen, J. M., Langer, W. D., Rosen, L. C., and Cameron, A. G. W.: 1969,Astrophys. Space Sci. 5, 113.
Das, P. K.: 1976,Monthly Notices Roy. Astron. Soc. 177, 391.
Durgapal, M. C. and Pande, A. K.: 1980,Ind. J. Pure Appl. Phys. 18, 171.
Durgapal, M. C., Pande, A. K., and Pandey, K.: 1979,J. Phys. A12, 859.
Goldreich, P. and Julian, H. W.: 1969,Astrophys. J. 157, 869.
Gunn, J. E. and Ostriker, J. P.: 1969,Astrophys. J. 157, 1395.
Harrison, K. K., Thorne, K. S., Wakano, M., and Wheeler, J. A.: 1965,Gravitation Theory and Graviational Collapse, Univ. of Chicago Press, Chicago, pp. 42, 50, and 156.
Hartle, J. B.: 1967,Astrophys. J. 50, 1005.
Hartle, J. B. and Sharpe, D. H.: 1965,Phys. Rev. Letters 15, 909.
Irvine, J. M.: 1978,Neutron Stars, Oxford University Press, Oxford, p. 152.
Leung, Y. C. and Wang, C. G.: 1971,Astrophys. J. 170, 499.
Misner, C. W., Thorne, K. S., and Wheeler, J. A.: 1973,Gravitation, W. H. Freeman and Comp., San Francisco, p. 621.
Oppenheimer, J. R. and Volkoff, G.: 1939,Phys. Rev. 55, 374.
Rees, M., Ruffini, R. and Wheeler, J. A.: 1974,Black Holes, Gravitational Waves and Cosmology — An Introduction to Current Research, Gordon and Breach, New York, p. 23.
Tolman, R. C.: 1934,Relativity, Thermodynamics, and Cosmology, Clarendon Press, Oxford, p. 247.
Zel'dovich, Ya. B.: 1962,Soviet Phys. JETP 14, 1143.
Zel'dovich, Ya. B. and Novikov, I. D.: 1971,Relativistic Astrophysics, Vol. I, Univ. of Chicago Press, Chicago, p. 286.
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Durgapal, M.C., Pande, A.K. & Rawat, P.S. Extreme relativistic model for neutron stars and pulsars. Astrophys Space Sci 90, 117–126 (1983). https://doi.org/10.1007/BF00651552
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DOI: https://doi.org/10.1007/BF00651552