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Published byWorld Scientific Publis
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viA. Ashtekarof space-time that eme
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viiiA. AshtekarGravitational waves
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xA. Ashtekarhappy, schizophrenic at
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xviContents9. Receiving Gravitation
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4 J. Stachel(2) the change over tim
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6 J. StachelFig. 2respectively. Fur
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8 J. Stachelof string theory, M-the
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10 J. StachelLogically, it would se
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12 J. Stachelupon by no (net) exter
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14 J. Stachelof the incompatibility
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16 J. Stachelis an important differ
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18 J. Stachelbetween physical conce
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20 J. Stachel10. Four-Dimensional F
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22 J. Stachelderivative of the metr
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24 J. Stachel(b) General relativity
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26 J. Stachelfour-dimensional analo
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28 J. Stachelply the lessons learne
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30 J. Stachelmanifold appropriate f
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32 J. Stachelwhich merely defines t
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34 J. Stacheldynamical process as a
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36 J. Stachel9. J. Stachel, Special
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Part IIEinstein’s UniverseRamific
- Page 58 and 59: 40 H. Nicolai• Higher dimensions
- Page 60 and 61: 42 H. Nicolaiadvance, and possibly
- Page 62 and 63: 44 H. NicolaiBianchi identities are
- Page 64 and 65: 46 H. NicolaiIt does not appear pos
- Page 66 and 67: 48 H. NicolaiThe other SL(2, R), of
- Page 68 and 69: 50 H. Nicolai3.1. BKL dynamics and
- Page 70 and 71: 52 H. Nicolaidegrees of freedom, th
- Page 72 and 73: 54 H. Nicolaiin the valley. The Ham
- Page 74 and 75: 56 H. NicolaiThe main feature of th
- Page 76 and 77: 58 H. Nicolai4. Basics of Kac Moody
- Page 78 and 79: 60 H. Nicolaifor indefinite A. It i
- Page 80 and 81: 62 H. NicolaiThe level l = 0 sector
- Page 82 and 83: 64 H. NicolaiConsequently, the repr
- Page 84 and 85: 66 H. Nicolaiwhere the abelian part
- Page 86 and 87: 68 H. Nicolaiconstant momenta Π yi
- Page 88 and 89: 70 H. Nicolaiσ-model side is suppo
- Page 90 and 91: 72 H. NicolaiReferences1. H.A. Buch
- Page 92 and 93: 74 H. Nicolai44. G. Neugebauer and
- Page 94 and 95: CHAPTER 3THE NATURE OF SPACETIME SI
- Page 96 and 97: 78 A. D. Rendallspacetime to define
- Page 98 and 99: 80 A. D. RendallOne of the most imp
- Page 100 and 101: 82 A. D. Rendalltheorems was an elu
- Page 102 and 103: 84 A. D. Rendallsymmetric solution
- Page 104 and 105: 86 A. D. Rendallback into a curvatu
- Page 106 and 107: 88 A. D. Rendallspace and there are
- Page 110 and 111: 92 A. D. Rendallmean curvature foli
- Page 112 and 113: 94 P. T. ChruścielHere dΩ 2 denot
- Page 114 and 115: 96 P. T. Chruścielr = constant < 2
- Page 116 and 117: 98 P. T. Chruścielthe formHereg =
- Page 118 and 119: 100 P. T. ChruścielFig. 3. A coord
- Page 122 and 123: 104 P. T. ChruścielRather surprisi
- Page 124 and 125: 106 P. T. ChruścielA key notion re
- Page 126 and 127: 108 P. T. ChruścielA simple exampl
- Page 128 and 129: 110 P. T. ChruścielVacuum or elect
- Page 130 and 131: 112 P. T. Chruścielangular momentu
- Page 132 and 133: 114 P. T. ChruścielRobinson-Trautm
- Page 134 and 135: 116 P. T. Chruścielto the past. Ho
- Page 136 and 137: 118 P. T. ChruścielBecause of the
- Page 138 and 139: 120 P. T. Chruścielde Witt, eds.),
- Page 140 and 141: 122 P. T. Chruściel54. J.B. Hartle
- Page 142 and 143: CHAPTER 5THE PHYSICAL BASIS OF BLAC
- Page 144 and 145: 126 R. H. Price2. Stationary Black
- Page 146 and 147: 128 R. H. Pricecan be dynamical in
- Page 148 and 149: 130 R. H. PriceThe physics of gravi
- Page 150 and 151: 132 R. H. PricecτEctCΑDCΒΑΒr g
- Page 152 and 153: 134 R. H. Pricebe thought of as a d
- Page 154 and 155: 136 R. H. Price(shown as the dotted
- Page 156 and 157: 138 R. H. PriceHere ψ is r 2 times
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140 R. H. Priceget within a distanc
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142 R. H. Priceopposite is true. Ne
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144 R. H. Priceviscous heating of t
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146 R. H. Priceof order of the grav
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148 R. H. PricetimehorizonCαBAFig.
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150 R. H. Priceform a hole. In term
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CHAPTER 6PROBING SPACE-TIME THROUGH
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154 P. Lagunaprovides a basic overv
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156 P. Lagunawas originally introdu
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158 P. LagunaWith the generalized h
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160 P. Lagunaimportance of the expl
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162 P. LagunaThe singularity has be
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164 P. Lagunafoliation. Even though
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166 P. Lagunaof attaching at the en
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168 P. LagunaAcknowledgmentsWork su
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170 P. Lagunainstances, 68,11 it is
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172 P. Laguna17. C. Bona, C. Ledvin
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174 P. Laguna63. S.A. Teukolsky. As
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176 T. PadmanabhanThese difficultie
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178 T. Padmanabhan(4) Combining the
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180 T. PadmanabhanWhen the δ ≪ 1
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182 T. Padmanabhan4. Inflation and
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184 T. PadmanabhanThis provides a g
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186 T. Padmanabhanat the end of inf
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188 T. PadmanabhanFig. 1. Different
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190 T. Padmanabhaneffects. In other
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192 T. Padmanabhandark energy using
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194 T. PadmanabhanOne key differenc
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196 T. Padmanabhana > a F . One can
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198 T. Padmanabhanlimit, the wave f
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200 T. Padmanabhanformal factor of
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202 T. Padmanabhanastro-ph/0411043;
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204 T. Padmanabhan37. A.D. Dolgov,
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206 C. M. Willadvance, and Joseph W
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208 C. M. Willated with dynamical f
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210 C. M. Willproposed NASA-ESA Sat
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19801970196019401920190019902000212
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214 C. M. WillA better bound on dα
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216 C. M. Willcurvature; J is the a
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218 C. M. WillFig. 3. Measurements
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220 C. M. WillTable 2. Parameters o
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222 C. M. Willcould differ from tha
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224 C. M. Willand 2.1 × 10 5 , dep
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226 C. M. Will40. T. Jacobson, S. L
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CHAPTER 9RECEIVING GRAVITATIONAL WA
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230 P. R. Saulsonfield equations, w
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232 P. R. Saulsona plane in space i
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234 P. R. SaulsonFig. 2. A schemati
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236 P. R. Saulsonbeam accumulates a
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238 P. R. SaulsonThat depends on wh
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240 P. R. Saulson6. Further Advance
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242 P. R. Saulson“waste” light
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244 P. R. SaulsonL = 500 m was adeq
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246 P. R. Saulsonbenefits. One was
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248 P. R. SaulsonASCLSCPSLIOO COC C
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250 P. R. Saulsonconstruction proje
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252 P. R. Saulsonpulsars), 25 quasi
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254 P. R. Saulsonplans to continue
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256 P. R. Saulson18. R. W. Drever,
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258 N. Ashbyincludes an almanac for
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260 N. Ashbyflawed technical report
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262 N. Ashbyestablished by the Bure
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264 N. Ashbyattempt this find that
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266 N. Ashbytransformations, and re
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268 N. AshbyBetter models can be fo
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270 N. AshbySimplify by writing the
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272 N. Ashbycan show that the total
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274 N. Ashbycentripetal potential (
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276 N. AshbyRms errors in TOPEX clo
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278 N. Ashbypotential V R (in ECI c
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280 N. Ashbyof clocks in GPS satell
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282 N. Ashbywhere a is the perturbe
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284 N. Ashbynominal semi-major axis
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286 N. AshbyEffect on Geodetic Dist
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288 N. Ashbymercial, private, and m
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294 L. H. FordIn this article, we w
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296 L. H. Fordsystem. (For example,
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298 L. H. Fordis vastly larger than
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300 L. H. Fordthe system be a super
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302 L. H. Fordinside the horizon. I
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304 L. H. Fordis that there is an i
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306 L. H. Fordfluctuations of space
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308 L. H. Fordand a more complete q
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310 L. H. Ford51. M. Alcubierre, Cl
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312 T. Banks1. IntroductionThe hist
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314 T. Banksobservable associated w
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316 T. BanksS int = µ p∫d σ a1
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318 T. BanksHowever, M2 branes wrap
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320 T. Banksto the gauge field stre
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322 T. Banksmoduli space. Indeed, t
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324 T. Banksform:KMV = e P 2 [K i¯
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326 T. Banksalgorithm for computing
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328 T. Banksinto the CFT statement
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330 T. Banksspace, have an AdS radi
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332 T. Banksthat there is a positiv
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334 T. Bankslandscape, while I go o
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336 T. Banksthen be viewed as an ou
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338 T. Banksto study. The covariant
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340 T. Banksit is probably necessar
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342 T. Banksbetween the dynamics in
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344 T. Banksthetical space-time pro
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346 T. Banks7. M.B. Green, J.H. Sch
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348 T. Banks40. K. Becker and M. Be
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CHAPTER 13QUANTUM GEOMETRY AND ITS
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352 A. Ashtekarfirst this similarit
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354 A. AshtekarThis chapter organiz
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356 A. Ashtekarsion is not renormal
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358 A. Ashtekarii) fluxes E S,t =
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360 A. AshtekarH. Furthermore detai
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362 A. Ashtekarwithout any referenc
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364 A. AshtekarTo summarize, from t
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366 A. AshtekarThis point is especi
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368 A. Ashtekargeometric operators.
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370 A. Ashtekarlevel and then quant
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372 A. Ashtekarfull theory, one can
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374 A. Ashtekarthe big bang but has
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376 A. AshtekarReuter have presente
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378 A. Ashtekarcontext of loop quan
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380 A. Ashtekardation, the Sir C.V.
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CHAPTER 14LOOP QUANTUM COSMOLOGYMAR
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384 M. Bojowaldton, in addition to
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386 M. Bojowaldsolution a ∝ exp(
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388 M. Bojowaldt. The latter fact i
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390 M. BojowaldThis shows that choo
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392 M. Bojowald(iii) only exponenti
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394 M. Bojowaldwell be formulated i
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396 M. Bojowaldstarts to break down
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398 M. Bojowaldwhich does not stop
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400 M. Bojowald4.3.1. QuantizationF
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402 M. Bojowald1.61.41.210.80.60.40
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404 M. BojowaldThe effective Friedm
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406 M. Bojowald181512a / l P963010
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aφ10500.5a/300408 M. Bojowald00 10
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410 M. Bojowaldsingularity. These f
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412 M. Bojowald4. D. N. Spergel et
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414 M. Bojowald61. G. V. Vereshchag
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416 R. Gambini and J. Pullinwidely
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418 R. Gambini and J. Pullin2. Cons
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420 R. Gambini and J. PullinTo clar
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422 R. Gambini and J. Pullinwith M
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424 R. Gambini and J. Pullin1q 10-1
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426 R. Gambini and J. Pullin0.020.0
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428 R. Gambini and J. Pullin0.020.0
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430 R. Gambini and J. Pullinmotion
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432 R. Gambini and J. PullinLet us
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434 R. Gambini and J. Pullin1.61.41
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436 R. Gambini and J. Pullinmeasure
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438 R. Gambini and J. Pullintransfo
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440 R. Gambini and J. PullinIn the
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442 R. Gambini and J. Pullinof q or
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444 R. Gambini and J. Pullintum Mec
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446 F. Dowkerspace could be reduced
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448 F. Dowkerthe fact that the two
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450 F. Dowkera Lorentzian metric te
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452 F. DowkerLet us therefore, in o
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454 F. Dowkerstructure is of three
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456 F. DowkerThe solution of these
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458 F. Dowkerof Now is special but
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460 F. DowkerEven if we had in hand
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462 F. Dowkerenergy. 10 A naive app
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464 F. Dowker16-21, 2001, Cambridge
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466 R. Penroseforms of the measurem
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468 R. PenroseZ ∈ N − I). There
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470 R. Penroseinfinity”). In view
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472 R. Penrosefor it to do so is
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474 R. PenroseFurthermore, it turns
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476 R. PenroseHere φ AB...L has
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478 R. Penroseof the homogeneities
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480 R. Penrosetation (perhaps even
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482 R. Penroseexamples of certain w
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484 R. Penrosecomponent which exten
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486 R. PenroseIn fact, we can use a
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488 R. Penroseculation to show that
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490 R. Penrose(the latter condition
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492 R. Penrosebe described. In such
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494 R. Penrosewhere we demand that
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496 R. Penrosecorresponding notion
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498 R. PenroseHowever, this is not
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500 R. PenroseEinstein case) it see
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502 R. Penrosekk. Witten (2003); th
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504 R. Penrose40. R. Penrose, Twist
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508 Indexdark energy, 298, 299decoh
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510 Indexrepulsion, 404resolution o