- Page 1: Université Paris Diderot UFR de Ph
- Page 6 and 7: ii Remerciements
- Page 8 and 9: iv TABLE DES MATIÈRES III Simulati
- Page 10 and 11: vi CV Adresse postale : LUTH Observ
- Page 12 and 13: viii Activités d’encadrement
- Page 14 and 15: x Résumé
- Page 16 and 17: xii Abstract
- Page 19 and 20: Introduction Des quatre interaction
- Page 21 and 22: Introduction 5 d’étude correspon
- Page 23: Première partie Formulation des é
- Page 26 and 27: 10 champ de vecteur n) et le temps
- Page 28 and 29: 12 l’intérieur de l’horizon (a
- Page 30 and 31: 14 Fully-constrained scheme (Bonazz
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36 Fully-constrained scheme (Bonazz
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38 Fully-constrained scheme (Bonazz
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40 Fully-constrained scheme (Bonazz
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42 Fully-constrained scheme (Bonazz
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44 Fully-constrained scheme (Bonazz
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46 Fully-constrained scheme (Bonazz
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48 Fully-constrained scheme (Bonazz
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50 Fully-constrained scheme (Bonazz
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52 Mathematical issues in a fully-c
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54 Mathematical issues in a fully-c
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56 Mathematical issues in a fully-c
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58 Mathematical issues in a fully-c
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60 Mathematical issues in a fully-c
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62 Mathematical issues in a fully-c
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64 Mathematical issues in a fully-c
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66 Mathematical issues in a fully-c
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68 Mathematical issues in a fully-c
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70 Improved constrained scheme. . .
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72 Improved constrained scheme. . .
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74 Improved constrained scheme. . .
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76 Improved constrained scheme. . .
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78 Improved constrained scheme. . .
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80 Improved constrained scheme. . .
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82 Improved constrained scheme. . .
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84 Improved constrained scheme. . .
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86 Improved constrained scheme. . .
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88 Improved constrained scheme. . .
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90 Improved constrained scheme. . .
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92 Improved constrained scheme. . .
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Les équations d’Einstein se pré
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parentes » pour que les ondes puis
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100 Spectral methods for numerical
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102 Spectral methods for numerical
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104 Spectral methods for numerical
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106 Spectral methods for numerical
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108 Spectral methods for numerical
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110 Spectral methods for numerical
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112 Spectral methods for numerical
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114 Spectral methods for numerical
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116 Spectral methods for numerical
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118 Spectral methods for numerical
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120 Spectral methods for numerical
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122 Spectral methods for numerical
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124 Spectral methods for numerical
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126 Spectral methods for numerical
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128 Spectral methods for numerical
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130 Spectral methods for numerical
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132 Spectral methods for numerical
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134 Spectral methods for numerical
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136 Spectral methods for numerical
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138 Spectral methods for numerical
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140 Spectral methods for numerical
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142 Spectral methods for numerical
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144 Spectral methods for numerical
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146 Spectral methods for numerical
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148 Spectral methods for numerical
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150 Spectral methods for numerical
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152 Spectral methods for numerical
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154 Spectral methods for numerical
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156 Spectral methods for numerical
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158 Spectral methods for numerical
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160 Spectral methods for numerical
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162 Spectral methods for numerical
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164 Spectral methods for numerical
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166 Spectral methods for numerical
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168 Spectral methods for numerical
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170 Spectral methods for numerical
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172 Spectral methods for numerical
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174 Spectral methods for numerical
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176 Spectral methods for numerical
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178 Spectral methods for numerical
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180 Spectral methods for numerical
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182 Spectral methods for numerical
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184 Spectral methods for numerical
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186 Spectral methods for numerical
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188 Spectral methods for numerical
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190 Absorbing boundary conditions.
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192 Absorbing boundary conditions.
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194 Absorbing boundary conditions.
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196 Absorbing boundary conditions.
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198 Absorbing boundary conditions.
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200 Absorbing boundary conditions.
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202 Divergence-free evolution. ..(N
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204 Divergence-free evolution. ..(N
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206 Divergence-free evolution. ..(N
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208 Divergence-free evolution. ..(N
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210 Divergence-free evolution. ..(N
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212 Divergence-free evolution. ..(N
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214 Divergence-free evolution. ..(N
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216 Divergence-free evolution. ..(N
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218 Divergence-free evolution. ..(N
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220 Divergence-free evolution. ..(N
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222 Divergence-free evolution. ..(N
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224 Divergence-free evolution. ..(N
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226 Apparent horizon finder (Lin &
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228 Apparent horizon finder (Lin &
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230 Apparent horizon finder (Lin &
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232 Apparent horizon finder (Lin &
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234 Apparent horizon finder (Lin &
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236 Apparent horizon finder (Lin &
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Après avoir détaillé les travaux
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Fig. III.1 - Lignes de champ magné
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de masse inférieure à la masse cr
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Chapitre 8 Combining spectral and s
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8.1 Introduction 247 in the deeper
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8.2 Physical model and equations 24
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8.2 Physical model and equations 25
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components, 8.2 Physical model and
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8.3 Numerical methods 255 in [148].
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domain 5 (fourth shell) 8.3 Numeric
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8.3 Numerical methods 259 - paralle
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8.3 Numerical methods 261 nonlinear
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8.3 Numerical methods 263 exact bou
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8.4 Code tests and applications 265
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8.4 Code tests and applications 267
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8.4 Code tests and applications 269
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β ϕ e [c] β ϕ e [c] -0.01 -0.02
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φ c | φ c 1/2 / φ c 3 - 1 | 1.06
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φ c φ r100 e 1.06 1.04 1.02 1.00
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ρ c [10 14 g cm -3 ] 4.0 3.0 2.0 1
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lhs φ , rhs φ lhs β 1, rhs β 1
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8.4 Code tests and applications 281
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v ϕ e [c] 0.4 0.3 0.2 0.1 8.4 Code
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8.4 Code tests and applications 285
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ρ c [10 14 g cm -3 ] 10.0 8.0 6.0
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8.5 Conclusions 289 We consider the
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8.A Differences to previous 2D CFC
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Chapitre 9 Rotating star initial da
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The evolution of the 3-metric γij
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with the conformal factor Ψ define
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9.2 Formulation 299 In summary, to
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9.3.2 Equation of state 9.3 Numeric
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9.3 Numerical results 303 Table 9.1
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9.4 Conclusion 305 Figure 9.4: Iso-
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9.4 Conclusion 307 Figure 9.7: Same
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9.A Resolution of the Poisson equat
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Chapitre 10 Relativistic numerical
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10.2 Canonical Two-Fluid Hydrodynam
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10.2 Canonical Two-Fluid Hydrodynam
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10.3 Stationary axisymmetric config
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10.3 Stationary axisymmetric config
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10.4 Numerical procedure 321 In gen
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10.5 Tests of the numerical code 32
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10.5 Tests of the numerical code 32
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log 10(⋄R) 0 -2 -4 -6 -8 -10 -12
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10.6 Numerical Results 329 very ast
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10.6 Numerical Results 331 that in
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10.7 Conclusions 333 Figure 10.8: C
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10.A The Newtonian analytic slow-ro
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10.A The Newtonian analytic slow-ro
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Calculating the Kepler-limit 10.A T
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Chapitre 11 The gyromagnetic ratio
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11.2 Model and assumptions 343 is t
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g−factor 1.5 1 11.3 Numerical stu
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g−factor 2 1.8 1.6 1.4 1.2 11.3 N
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g−factor 1.645 1.64 1.635 11.3 Nu
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11.4 Conclusions 351 who calculated
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Chapitre 12 Velocity-induced collap
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12.2 Evolution of spherically symme
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12.3 Dynamical scenarios 357 Figure
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12.4 Numerical results 359 km. The
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Amplitude of initial velocity profi
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12.5 Summary and conclusions 363 di
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Chapitre 13 Excised black hole spac
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13.2 Isolated horizons as a local d
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[35]): 13.3 A fully constrained for
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13.3 A fully constrained formalism
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13.4 Boundary conditions and resolu
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13.4 Boundary conditions and resolu
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13.5 Numerical results and tests 13
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Values in geometrical units 1 0 13.
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13.5 Numerical results and tests 38
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Relative error with respect to Kerr
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13.A Tensor spectral quantities ada
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13.B Recovery of h ij from A and ˜
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Conclusions Ce manuscrit détaille
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Perspectives Interaction d’un tro
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Perspectives 393 A. Mezzacappa à O
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Liste des publications Revues à co
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T.Contini, J.M. Hameury, L. Pagani,
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Bibliographie [1] Abbott, B., Abbot
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BIBLIOGRAPHIE 401 [28] Ansorg, M.,
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BIBLIOGRAPHIE 403 [60] Ben Belgacem
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BIBLIOGRAPHIE 405 [93] Brun, A. S.,
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BIBLIOGRAPHIE 407 [125] Comer, G. L
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BIBLIOGRAPHIE 409 [157] Donat, R.,
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BIBLIOGRAPHIE 411 [189] Friedrich,
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BIBLIOGRAPHIE 413 [221] Gourgoulhon
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BIBLIOGRAPHIE 415 [255] Holst, M.,
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BIBLIOGRAPHIE 417 [287] Langlois, D
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BIBLIOGRAPHIE 419 [319] Misner, C.
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BIBLIOGRAPHIE 421 [352] Ott, C. D.,
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BIBLIOGRAPHIE 423 [384] Regge, T. e
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BIBLIOGRAPHIE 425 [415] Shibata, M.
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BIBLIOGRAPHIE 427 [448] Szilágyi,
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BIBLIOGRAPHIE 429 [479] Wald, R. M.