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A A new conjecture on the micro states of black-holes

  1. Feb 21, 2017 #1
    Dear All Gravitinos,

    I write this post here to discuss a new conjecture on resolutions of the schwarzschild singularity and the physic interpretation for the micro states of black-holes (arxiv: 1606.06178, published in Nucl. Phys. B2017,02,005, http://dx.doi.org/10.1016/j.nuclphysb.2017.02.005).

    In this paper I quotient an idea that: matters inside the horizon of schwarzschild black-holes are not concentrating on the central point, instead they are dispersed inside the horizon and are experiencing repeated motion of contraction and over-head — anti-directional expansion — contraction again. I provide numerical evidences at both general relativity and quantum gravitation levels that, the modes of matter distributions inside the horizon is of order exp(A/l_pl^2). This idea resolves the scharzschild singularity but avoids contradictions with the singularity theorem and provides an intuitive explanation for the origin of black-hole entropy, and very probably a method of resolving the information missing puzzle involved in the hawking radiations.

    I expect this picture is dis/verifiable since in the mergering of binary black-holes, gravitation waves coming from the binary mass-points covered by horizon and those from binary mass-distributions also covered by horizon should be distinguishable.

    How do you, all gravitation and black-hole professionals look about this idea? I know some big mans in this area are in this forum
    Last edited: Feb 21, 2017
  2. jcsd
  3. Feb 21, 2017 #2
    Well, as distinct from a big man, I'm only a lay person who has read plenty including Thorne's Black Holes and Time Warps, and Rees and Begalman's "Gravity's Fatal Attraction", but I 'm certain that GR tells us that once the Schwarzchild radius is reached in any matter, that further collapse is compulsory, at least up to the quantum/Planck level where GR is not applicable.
    Most Physicists do not believe that any physical singularity is reached, and a future QGT may reveal more in that regard.
  4. Feb 22, 2017 #3
    My key observation is, to reveal more in the further collapse after the schwarzschild radius is reached, the usual general relativity and canonical quantum gravitation may be enough.

    To see this clearly, we only need to know a fact that, the very large black holes have very small average mass densities. So, if we consider the inverse-time evolution of our universe, when its density reaches about 0.02g/cm^3[=M_milk/(4pi*/3*(2GM_milk/c^2)^3)], the spherical region as large as our milky way centered on us has become in the horizon of a black hole. However, this does not prohibit cosmologists to use general relativity to study its evolutions at all. The key point here is, choosing an appropriate time coordinates.

    In our papers, we choose a time coordinate very similar to the co-moving time of cosmologists, so that evolutions after the horizon forms can still be explored conveniently in general relativity and canonical quantum gravitations.
    Last edited: Feb 22, 2017
  5. Feb 22, 2017 #4


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    2016 Award

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    How accessible is this to the existing gravitational wave observatories? You mention a difference in black hole mergers. The ringdown has been observed already, how do you have any estimate how much it changes in your model?
  6. Feb 22, 2017 #5
    Currently, I did no numerical simulations about the gravitational waves following from binary black holes with non-trivial inner mass distribution. But I indeed read most of the existing literatures studying this subject. All of them seem to take the inner part of merging black holes as simple mass point covered by horizons. In their numerical codes, the inner part of black holes are all excised simply and imposes no effects on the form of gravitational waves they predicted. One of my purposes of posting this thread here is to attract attentions from professionals in this area, if they can/already do this simulation and give definite predictions, the fact will become very interesting for the near future gravitational wave observations.
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