Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001ap%26ss.275..185n&link_type=abstract
Astrophysics and Space Science, v. 275, Issue 3, p. 185-207 (2001).
Astronomy and Astrophysics
Astrophysics
2
Scientific paper
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_crit <= (5/3) (for which a supermassive star represent neutrally stable system), the mass, and the size of this object comes out to be 6.87 × 10^7 M_solar <= M <= 1.7 × 10^9M_solar, and 2.74× 10^14 cm <= a <= 1.43× 10^15cm respectively, for the central temperature, T_0 = 6× 10^7°K, which is sufficient for the release of nuclear energy. The total energy released during their evolution ranges from 2.46× 10^60 - 3.18× 10^62 erg, which is sufficient to power these objects at least for a period of ~ 10^6 - 10^7 years. These figures agrees quite well with those cited for Quasi Stellar Objects (QSOs) in the literature.
Durgapal M. C.
Negi P. S.
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