Raknath,
What I said was in response to Philose who said
Philose said:
So I am defiantly no scientist and I don's know much so ...
It has been said that the black holes take in everything and ... then wouldn't information be jumped out another side? It would seem like a explosion from a single point like the big bang states...
So my question is, could this be possible or is this even reasonably stated?
Philose on his own came up with an idea similar to Smolin's CNS---a spacetime region branching, reproducing itself via black hole big bangs. He was thinking about it in general nontechnical terms. So I tried to give as complete and honest a response as I could without putting him off by excessive technicality.
You are asking questions on a different plane, now. You want more detail. Everything should be said in a different, more precise vocabulary. We might need to start a new thread.
There are various different approaches to QG. Which one or ones would you like to know about? What would you like to know?
About discretizing---if that is an issue for you. In Loop the basis is a smooth manifold. You build on that. The math model of space is not divided up into little bits. The math model of space time is also not divided up into little bits.
However certain observables, corresponding to geometric measurements, are represented by operators on a hilbertspace. These operators have discrete spectra. In that sense the continuum is smooth but like "energy levels" in the hydrogen atom when you make a measurement of something you can get discrete levels (like of area).
The situation in Loop turns out to be consistent with Lorentz invariance, i.e. with special rel. Rovelli has a 2002 paper about this. If you want a link please ask.
In another approach, Triangulations (see the SciAm article in my sig, by Loll) the basic spacetime is also a continuum. You divide it up, for convenience, into little pieces, but then you let the size of the pieces go to zero. You don't imagine that space is itself divided up. You just use the division as a temporary tool for calculation and for computer simulations of universes.
I hope that replies to your concern about discreteness, or space being made of little bits.
In QG it ordinarily is not (Atyy pointed to some variant QGs where it is little bits, but that isn't typical).
Then you had a question about entropy.
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There is a serious technical issue about entropy and the Second Law re bounce cosmologies. I can't resolve it. Penrose pointed out the problem and I don't quite follow either his definition of the entropy of the gravitational field or his extension of the Second Law to cover this case. It may be that he does not actually have a rigorous well-founded argument. But I've heard him make the argument in person, and also several times in video lectures. The best I can do here is to discuss it at an intuitive level.
The key thing there is how one defines the entropy of the gravitational field. As I recall, according to Penrose low entropy corresponds to a smooth uniform gravitational field---before any clumping/coagulation has taken place. The blank even field is the state of highest order, and as stars and galaxies and clusters of galaxies curdle and coagulate it represents increasing disorder in the grav field. Increasing grav entropy.
This may seem paradoxical: the entropy of matter behaves differently--- picture gas in a box. If it starts clumped in one corner that is low entropy and as it spreads out uniformly to fill the box evenly, the entropy increases. Penrose stressed that, visually, gravitational entropy behaves in a way that is opposite to matter entropy.
Now he says: in a bounce you have a bumpy disorderly geometry (an old universe where matter has condensed into stars) that collapses and produces a smooth blank expanding geometry---it looks like you have gone from high entropy to a low.
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I have several questions about this. One is, who is the observer? I think measuring entropy implicitly requires an observer and the Second Law says that the observer will (almost) never see entropy decrease. In a bounce, the observer has to be either before or after and neither Mr Before or Mr After will actually witness a violation.
I also have a problem with how Penrose defines the entropy of the universe because I'm used to imagining an enclosed system from some outside observer's perspective and universe doesn't provide an outside.But the main difficulty I have is that this whole doctrine assumes that gravity is always attractive! That is the only reason you can say that the clumped bumpy uneven field is higher entropy than the smooth. Because since gravity is attractive, as time goes on there will always be more and more clumping and dissipation of energy as lowgrade heat.
But the tables are turned if gravity briefly turns repulsive. (This occurs in quantum cosmology models at very high, near-Planck, density.) In that case everything wants to spread out evenly instead of clump. The equilibrium high entropy state is then the uniform one---which however counts as low entropy when the system expands enough for gravity to become attractive again.
I think one way to sum this up is to say that entropy is itself observer dependent. It depends on what standpoint. Is the observer before the bounce looking into the future, or after the bounce looking back into the past. Perhaps neither one can see a violation of the Second Law. And if no one sees a violation, then the Second Law was not violated.
I'm not sure about this. I am speculating to some extent. These are just some things to think about. Perhaps we can continue later, as time permits.