I will quote him, with his permission: ", I gave a talk a few months ago at P.I. on my research on finite states in QGRA. It was realized during the talk that I would have had to have solved the initial value problem of GR, in order to quantize it by my method. They didn't believe it at first, since GR is a major problem which apparently nobody knows how to solve. So they made me show them. After I did, I'm not sure if they believed it totally, but certainly they began to see how it could be plausible: which Lee Smolin himself admitted. Laurent Friedel at first thought I must be completely wrong, but then changed his view from me as a guy making ludicrous claims, to the more open-minded possibility that I could have something there after I sketched out a few lines. They asked me to write up a sketch of the proof, as it would be a significant discovery. I gave them a 70 page paper outlining some of the basics, without giving it completely away, at least to let the P.I. group could digest it. So far, after several months, they are still trying to come to grips with the procedure: but have not yet come back to say that I'm wrong- or right: I have challenged Friedel to prove me wrong, but so far he hasn't: and likewise with Smolin and some other P.I. members. I've been holding off on posting my solution, to give P.I. the chance to come to a definie conclusion: but I might just go ahead and post it so that others can have a chance to see it: since I'd like to get some feedback. The classical solution is an intermediate step in my quantum solution: but I understand that many people are interested in the classical aspects as well. It has to do with a set of new variables I've developed in QGRA. The `momentum' variable, which is essentially the antiself-dual part of the Weyl curvature tensor, has taken on a completely new interpretation. One of the properties it encodes about a spacetime is the amount of anisotropy, which has observational implications: amongst the things I've worked out include ways of testing the semiclassical limit of QGRA without needing to go all the way to the Planck scale- this limit would leave its imprint on these variables in ways which would stick out possibly at every day energy scales. The anisotropy in this tensor is in an internal SU(2) space, but can be transformed into spacetime by my procedure for constructing GR solutions. One thing it could potentially be used to corroborate is the anisotropy in the CMB temperature spectrum, and relate that to quantum cosmology. Nonetheless, I would be cautious in saying that they can't prove me wrong: so far, P.I. has not yet arrived at a definite conclusion. The nature from their perspective is such that it takes time, intense concentration and rigor, and resources to get a handle on, and there are no shortcuts." I have the sketch of the full paper.