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Masses of radiation pressure supported stars in extreme relativistic realm

Published online by Cambridge University Press:  01 August 2006

Abhas Mitra
Abhas Mitra*
Affiliation:
Theoretical Astrophysics Section, BARC, Mumbai-400085, India email: abhasmitra@rediffmail.com
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Abstract

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We discuss that in the extreme relativistic limit, i.e., when z ≫ 1, where z is the surface gravitational redshift, there could be radiation pressure supported and dominated stars with arbitrary gravitational mass, high or low. Such objects are called Eternally Collapsing Objects (ECOs). ECOs are practically as compact as Schwarzschild black holes (BH) and, observationally, are likely to be mistaken as BHs. Further since any object undergoing continued collapse must first become an ECO before becoming a true BH state characterized by M = 0, the observed BH Candidates are ECOs.

Keywords

Gravitation – black holes
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S238: Black Holes from Stars to Galaxies – Across the Range of Masses , August 2006 , pp. 409 - 410
Copyright
Copyright © International Astronomical Union 2007

References

Mitra, A. 2006a, MNRAS, 367, L66, gr-qc/0601025CrossRefGoogle Scholar
Mitra, A. 2006b, MNRAS, 369, 492, gr-qc/0603055CrossRefGoogle Scholar
Mitra, A. 2006c, PRD, 74, 024010, gr-qc/0605066CrossRefGoogle Scholar
Mitra, A. 2006d, New Astronomy, 12, 146, astro-ph/0608178CrossRefGoogle Scholar
Mitra, A. 2006e, PRD, in press, gr-qc/0607087Google Scholar
Mitra, A. 2006f, Adv. Sp. Res., in press, astro-ph/0510162Google Scholar
Mitra, A. 2005, physics/0504076Google Scholar
Mitra, A. 2002, Found. Phys. Lett., 15, 439, astro-ph/0207056CrossRefGoogle Scholar
Mitra, A. 2004, astro-ph/0408323Google Scholar
Robertson, S. L. & Leiter, D. J. 2002, ApJ, 565, 447, astro-ph/0102381CrossRefGoogle Scholar
Robertson, S. L. & Leiter, D. J. 2003, ApJL, 596, L203, astro-ph/0310078CrossRefGoogle Scholar
Robertson, S. L. & Leiter, D. J. 2004, MNRAS, 350, 1391, astro-ph/0402445CrossRefGoogle Scholar
Robertson, S. L. & Leiter, D. J. 2006, astro-ph/0603746Google Scholar
Schild, R. E., Leiter, D. J. & Robertson, S. L. 2006, AJ, 132, 420, astro-ph/0505518CrossRefGoogle Scholar