Relativistic supermassive stars

A plausible scenario for the formation of a stable supermassive star in the relativistic regime has been discussed. The onset of the negativity of the `distribution function' in the stable sequences of the star clusters [the stability of star clusters is assured by using the variational method...

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Bibliographic Details
Published in:Astrophysics and space science 2001-02, Vol.275 (3), p.185
Main Authors: Negi, Ps, Durgapal, Mc
Format: Article
Language:English
Subjects:
Astrophysics
Stars & galaxies
Online Access:Get full text
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Summary:A plausible scenario for the formation of a stable supermassive star in the relativistic regime has been discussed. The onset of the negativity of the `distribution function' in the stable sequences of the star clusters [the stability of star clusters is assured by using the variational method (Chandrasekhar, 1964a,b) for equivalent gas spheres] described by Tolman's type VII solution with vanishing surface density has been regarded as an indication of the conversion of the cluster structure into a supermassive star. For the critical values of the `adiabatic index', (4/3) < γ^sub crit^ ≤ (5/3) (forwhich a supermassive star represent neutrally stable system), the mass, and the size of this object comes out to be 6.87 × 10^sup 7^ M^sub ^ ≤M ≤ 1.7 × 10^sup 9^M^sub ^, and 2.74× 10^sup 14^ cm ≤ a≤ 1.43× 10^sup 15^cm respectively, for the central temperature,T^sub 0^ = 6× 10^sup 7^°K, which is sufficient for the release ofnuclear energy. The total energy released during their evolution rangesfrom 2.46× 10^sup 60^ - 3.18× 10^sup 62^ erg, which is sufficient to power these objects at least for a period of 10^sup 6^ - 10^sup 7^years. These figures agrees quite well with those cited for Quasi Stellar Objects (QSOs) in the literature.[PUBLICATION ABSTRACT]
ISSN:0004-640X
1572-946X
DOI:10.1023/A:1002707730439