Radiation Pressure Supported Stars in Einstein Gravity: Eternally Collapsing Objects
arXiv:gr-qc/0603055 · doi:10.1111/j.1365-2966.2006.10332.x
Abstract
Even when we consider Newtonian stars, i.e., stars with surface gravitational redshift, z<< 1, it is well known that, theoretically, it is possible to have stars, supported against self-gravity, almost entirely by radiation pressure. However, such Newtonian stars must necessarily be supermassive. We point out that this requirement for excessive large M, in Newtonian case, is a consequence of the occurrence of low z<< 1. On the other hand, if we remove such restrictions, and allow for possible occurrence highly general relativistic regime, z >> 1, we show that, it is possible to have radiation pressure supported stars at arbitrary value of M. Since radiation pressure supported stars necessarily radiate at the Eddington limit, in Einstein gravity, they are never in strict hydrodynamical equilibrium. Further, it is believed that sufficiently massive or dense objects undergo continued gravitational collapse to the Black Hole stage characterized by z =infty. Thus, late stages of Black Hole formation, by definition, will have, z >> 1, and hence would be examples of quasi-stable general relativistic RPSSs. This result is also supported by with our previous finding that that trapped surfaces are not formed in gravitational collapse and the value of the integration constant in the vacuum Schwarzschild solution is zero. Hence the supposed observed BHs are actually ECOs.
Minor chages in proof. Discusses why the observed BHs are actually ECOs and Chandrasekhar limit is not applicable to them
References in corpus (1)
Cited by in corpus (3)
- Why Gravitational Contraction Must be Accompanied by Emission of Radiation Both in Newtonian and Einstein Gravity
- Sources of Stellar Energy, Einstein- Eddington Timescale of Gravitational Contraction and Eternally Collapsing Objects
- Masses of radiation pressure supported stars in extreme relativistic realm