G'day from the land of ozzzz
This paper maybe of interest to the topic. The ABS is explains the point without further writting.
[astro-ph/9910408] Non-occurrence of trapped surfaces and Black Holes in spherical gravitational collapse: An abridged version
Non-occurrence of trapped surfaces and Black Holes in spherical gravitational collapse: An abridged version
Authors: Abhas Mitra (BARC, Theory Division)
(Submitted on 22 Oct 1999 (v1), last revised 5 Dec 2000 (this version, v5))
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Abstract: We have shown in that for arbitrary EOS and radiation transport properties, (even) the idealized spherical gravitational collapse DOES NOT lead to the formation of trapped surfaces: 2GM(r,t)/R <=1. Hence all singularity theorems of Hawking, Penrose and Geroch, built on the assumption of formation of trapped surfaces, get invalidated! And this inequality, demands that M->0 if indeed R->0. We have shown that the final state corresponds to a zero mass BH state and, this state would occur only after infinite proper time indicating that GR is indeed the only naturally singularity free theory for isolated bodies (as was cherished by Einstein). This M->0 state would materialize after the body radiates its entire initial mass-energy. Thus there is no event horizon at any finite R or M, and, therefore all the great theoretical confusions like whether there could be (i) White Holes, (ii) whether t (R) becomes spacelike (timelike) inside the EH (iii) Loss of information in gravitational collapse, and (iv) validity of cosmic censorship conjecture get resolved. At any finite proper time, the collapsed object would be either static (z<2) or may appear static (R almost frozen) though, in extreme cases, internally, in terms of proper radial length, it might be collapsing at a speed ~c! We call the latter as Eternally Collapsing Objects.
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later 2006 he writes this paper.
Sources of Stellar Energy, Einstein- Eddington Timescale of Gravitational Contraction and Eternally Collapsing Objects
[astro-ph/0608178] Sources of Stellar Energy, Einstein- Eddington Timescale of Gravitational Contraction and Eternally Collapsing Objects
Authors: Abhas Mitra
(Submitted on 8 Aug 2006 (v1), last revised 3 Sep 2006 (this version, v3))
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Abstract: We point out that although conventional stars are primarily fed by burning of nuclear fuel at their cores, in a strict sense, the process of release of stored gravitational energy, known as, Kelvin - Helmholtz (KH) process is either also operational albeit at an arbitrary slow rate, or lying in wait to take over at the disruption of the nuclear channel. In fact, the latter mode of energy release is the true feature of any self-gravity bound object including stars. We also highligh the almost forgotten fact that Eddington was the first physicist to introduce Special Relativity into the problem and correctly insist that, actually, total energy stored in a star is not the mere Newtonian energy but the total mass energy (E = M c^2). Accordingly, Eddington defined an ``Einstein Time Scale'' of Evolution where the maximum age of the Sun turned out to be t_E = 1.4. 10^{13} yr. We extend this concept by introducing General Relativity and show that the minimum value of depletion of total mass-energy is t_E =infty not only for Sun but for and sufficiently massive or dense object. We propose that this time scale be known in the name of ``Einstein - Eddington''. We also point out that, recently, it has been shown that as massive stars undergo continued collapse to become a Black Hole, first they become extremely relativistic Radiation Pressure Supported Stars. And the life time of such relativistic radiation pressure supported compact stars is indeed dictated by this Einstein -Eddington time scale whose concept is formally developed here. Since this observed time scale of this radiation pressure supported quasistatic state turns out to be infinite, such objects are called Magnetospheric Eternally Collapsing Objects (MECO).
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My question to this is what is the state or phase of matter in these star cores to be able to store gravitational radiation?
