# The fallacy of Oppenheimer Snyder collapse: no general relativistic collapse at all, no black hole, no physical singularity

@article{Mitra2011TheFO,
title={The fallacy of Oppenheimer Snyder collapse: no general relativistic collapse at all, no black hole, no physical singularity},
author={Abhas Mitra},
journal={Astrophysics and Space Science},
year={2011},
volume={332},
pages={43-48}
}
• A. Mitra
• Published 29 December 2010
• Physics
• Astrophysics and Space Science
By applying Birkhoff’s theorem to the problem of the general relativistic collapse of a uniform density dust, we directly show that the density of the dust ρ=0 even when its proper number density n would be assumed to be finite! The physical reason behind this exact result can be traced back to the observation of Arnowitt et al. (Phys. Rev. Lett. 4: 375, 1960) that the gravitational mass of a neutral point particle is zero: m=0. And since, a dust is a mere collection of neutral point particles…
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## References

SHOWING 1-10 OF 26 REFERENCES
The Mass of the Oppenheimer-Snyder Black Hole
The only instance when the General Relativistic (GTR) collapse equations have been solved (almost) exactly to explicitly find the metric coefficients is the case of a homogeneous spherical dust
A generic relation between baryonic and radiative energy densities of stars
By using elementary astrophysical concepts, we show that for any self-luminous astrophysical object the ratio of radiation energy density inside the body (ρr) and the baryonic energy density (ρ0) may
Quantum information paradox: Real or fictitious?
One of the outstanding puzzles of theoretical physics is whether quantum information indeed gets lost in the case of black hole (BH) evaporation or accretion. Let us recall that quantum mechanics
No uniform density star in general relativity
As per general relativity (GR), there cannot be any superluminal propagation of energy. And thus, the sound speed in a continuous medium, $c_{s}=\sqrt{dp/d\rho}$, must be subluminal. However, if one
Radiation pressure supported stars in Einstein gravity: eternally collapsing objects
Even when we consider Newtonian stars, that is, stars with surface gravitational redshift z « 1, it is well known that, theoretically, it is possible to have stars supported against self-gravity
On Continued Gravitational Contraction
• Physics
• 1939
When all thermonuclear sources of energy are exhausted a sufficiently heavy star will collapse. Unless fission due to rotation, the radiation of mass, or the blowing off of mass by radiation, reduce
Likely formation of general relativistic radiation pressure supported stars or ‘eternally collapsing objects’
• Physics
• 2010
Hoyle & Folwler showed that there could be Radiation Pressure Supported Stars (RPSS) even in Newtonian gravity. Much later, Mitra found that one could also conceive of their General Relativistic (GR)
RELATIVISTIC EQUATIONS FOR ADIABATIC, SPHERICALLY SYMMETRIC GRAVITATIONAL COLLAPSE
• Physics
• 1964
The Einstein equations for a spherically symmetrical distribution of matter are studied. The matter is described by the stress-energy tensor of an ideal fluid (heat flow and radiation are therefore
Why gravitational contraction must be accompanied by emission of radiation in both Newtonian and Einstein gravity
By using virial theorem, Helmholtz and Kelvin showed that the contraction of a bound self-gravitating system must be accompanied by release of radiation energy irrespective of the details of the