NON-OCCURRENCE OF TRAPPED SURFACES AND BLACK HOLES IN SPHERICAL GRAVITATIONAL COLLAPSE

@article{Mitra1998NONOCCURRENCEOT,  title={NON-OCCURRENCE OF TRAPPED SURFACES AND BLACK HOLES IN SPHERICAL GRAVITATIONAL COLLAPSE},  author={Abhas Mitra},  journal={Foundations of Physics Letters},  year={1998},  volume={13},  pages={543-579},  url={https://api.semanticscholar.org/CorpusID:13945362}}
  • A. Mitra
  • Published10 October 1998
  • Physics
  • Foundations of Physics Letters
AbstractBy using the most general form of Einstein equations for General Relativistic (GTR) spherical collapse of an isolated fluid having arbitrary equation of state and radiation transport properties, we show that they obey a Global Constraint, 2GM(r, t)/R(r, t)c2≤1, where R is the “invariant circumference radius”, t is the comoving time, and M(r, t) is the gravitational mass enclosed within a comoving shell r. This inequality specifically shows that, contrary to the traditional intuitive… 

34 Citations

Does the Principle of Equivalence Prohibit Trapped Surfaces from Forming in the General Relativistic Collapse Process?

It has recently been shown that time-like spherical collapse of a physical fluid in General Relativity does not permit formation of “trapped surfaces.” This result followed from the fact that the

A Model of Dust-like Spherically Symmetric Gravitational Collapse without Event Horizon Formation

Some dynamical aspects of gravitational collapse are explored in this paper. A timedependent spherically symmetric metric is proposed and the corresponding Einstein field equations are derived. An

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

On the final state of spherical gravitational collapse

Following our recent finding [1] that, for the final state of continued spherical gravitational collapse of sufficiently massive bodies, the final gravitational mass of the fluidMƒ → 0, we show that

A Model of Dustlike Spherically Symmetric Gravitational Collapse without Event Horizon Formation

Some dynamical aspects of gravitational collapse are explored in this paper. A time-dependent spherically symmetric metric is proposed and the corresponding Einstein field equations are derived. An

DOES PRESSURE ACCENTUATE GENERAL RELATIVISTIC GRAVITATIONAL COLLAPSE AND FORMATION OF TRAPPED SURFACES

It is widely believed that though pressure resists gravitational collapse in Newtonian gravity, it aids the same in general relativity (GR) so that GR collapse should eventually be similar to the

The Euclidean gravitational action as black hole entropy, singularities, and spacetime voids

We argue why the static spherically symmetric vacuum solutions of Einstein’s equations described by the textbook Hilbert metric g μ ν ( r ) is not diffeomorphic to the metric g μ ν ( ∣ r ∣ )

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

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

Mass of Schwarzschild Black Holes Is Indeed Zero And Black Hole Candidates Are Quasi Black Holes.

A Schwarzschild Black Hole (BH) is the gravitational field due to a neutral point mass, and it turns out that the gravitational mass of a neutral point mass: $M=0$ (Arnowitt, Deser, Misner, PRL 4,

60 References

RELATIVISTIC EQUATIONS FOR ADIABATIC, SPHERICALLY SYMMETRIC GRAVITATIONAL COLLAPSE

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

On Continued Gravitational Contraction

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

Universality and scaling in gravitational collapse of a massless scalar field.

Evidence is presented in support of conjectures that (1) the strong-field evolution in the p→p * limit is universal and generates structure on arbitrarily small spatiotemporal scales and (2) the masses of black holes which form satisfy a power law M BH ∞|p-p * | γ , where γ≃0.37 is a universal exponent.

The Large Scale Structure of Space-Time

The theory of the causal structure of a general space-time is developed, and is used to study black holes and to prove a number of theorems establishing the inevitability of singualarities under certain conditions.

Cosmic censorship and the role of pressure in gravitational collapse

Assuming the weak energy condition, we study the nature of the non-central shell-focusing singularity which can form in the gravitational collapse of a spherical compact object in classical general

On Massive neutron cores

It has been suggested that, when the pressure within stellar matter becomes high enough, a new phase consisting of neutrons will be formed. In this paper we study the gravitational equilibrium of

Precursory singularities in spherical gravitational collapse.

General conditions are developed for the formation of naked precursory singularities in spherical gravitational collapse and it is argued that they may well be an essentially generic feature of relativistic gravitational collapse.

Violation of cosmic censorship in the gravitational collapse of a dust cloud

The behaviour of the outgoing light rays in the gravitational collapse of an inhomogeneous spherically symmetric dust cloud is analyzed. It is shown that, for an open subset of initial density

Are Q‐stars a serious threat for stellar‐mass black hole candidates?

We examine the status of the threat posed to stellar-mass black hole candidates by the possible existence of Q-stars (compact objects with an exotic equation of state that might have masses well
...

Related Papers

Showing 1 through 3 of 0 Related Papers