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Cosmology Cosmological solutions of
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Cosmology Cosmological solutions of
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Cosmology claimed to represent the
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Cosmology claimed to represent the
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Cosmology claimed to represent the
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Cosmology A) Empty Worlds, vacuum e
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Cosmology A) Empty Worlds, vacuum e
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Cosmology The general solution is S
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Cosmology The general solution is S
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Cosmology The general solution is S
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Cosmology (d) Λ > 0 , k = 0: S = e
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Cosmology (d) Λ > 0 , k = 0: S = e
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Cosmology (d) Λ > 0 , k = 0: S = e
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Cosmology Terminology: Λ > 0 , k =
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Cosmology Terminology: Λ > 0 , k =
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Cosmology Terminology: Λ > 0 , k =
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Cosmology B) Matter dominated: ρ >
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Cosmology B) Matter dominated: ρ >
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Cosmology ct = C arcsin √ X −
- Page 39 and 40: Cosmology ct = C arcsin √ X −
- Page 41 and 42: Cosmology ct = C arcsin √ X −
- Page 43 and 44: Cosmology In each case we have S (t
- Page 45 and 46: Cosmology In each case we have S (t
- Page 47 and 48: Cosmology In each case we have S (t
- Page 49 and 50: Cosmology Einstein-de Sitter univer
- Page 51 and 52: Cosmology Einstein-de Sitter univer
- Page 53 and 54: Cosmology t = 2 3 H−1 (t) (EdS) H
- Page 55 and 56: Cosmology t = 2 3 H−1 (t) (EdS) H
- Page 57 and 58: Cosmology Back to the non-flat geom
- Page 59 and 60: Cosmology Back to the non-flat geom
- Page 61 and 62: Cosmology in terms of the observabl
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- Page 69 and 70: Cosmology The conclusion of the abo
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- Page 75 and 76: Cosmology C) Radiation dominated: p
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- Page 79 and 80: Cosmology C) Radiation dominated: p
- Page 81 and 82: Cosmology ❖ k = 0 : S (t) = 4 ¯
- Page 83 and 84: Cosmology In each case we have S (t
- Page 85 and 86: Cosmology In each case we have S (t
- Page 87 and 88: Cosmology In each case we have S (t
- Page 89: Cosmology κ ρ(t) = 3 H2 (t) K(t)
- Page 93 and 94: Cosmology Actually, in the radiatio
- Page 95 and 96: Cosmology 8π hν ργ(ν) dν = 3
- Page 97 and 98: Cosmology 8π hν ργ(ν) dν = 3
- Page 99 and 100: Cosmology Since ρ(t)S (t) 4 = ρ0S
- Page 101 and 102: Cosmology c○ 2009, F. Jegerlehner
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- Page 105 and 106: Cosmology T0 = (2.725 ± 0.002) ◦
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- Page 109 and 110: Cosmology However, the evolution of
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- Page 113 and 114: Cosmology ρ(t) Big Bang radiation
- Page 115 and 116: Cosmology The critical energy densi
- Page 117 and 118: Cosmology The critical energy densi
- Page 119 and 120: Cosmology The critical energy densi
- Page 121 and 122: Cosmology Ω0 = 1 c○ 2009, F. Je
- Page 123 and 124: Cosmology Ω0 = 1 is the critical
- Page 125 and 126: Cosmology Ω0 = 1 is the critical
- Page 127 and 128: Cosmology Ω0 = 1 is the critical
- Page 129 and 130: Cosmology ˙S 2 c 2 + k = κ 3 ρ S
- Page 131 and 132: Cosmology ˙S 2 c 2 + k = κ 3 ρ S
- Page 133 and 134: Cosmology q0 = κ (ρ0+3 p0) 6 H 2
- Page 135 and 136: Cosmology Form of energy equation o
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Cosmology in which case, independen
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Cosmology in which case, independen
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Cosmology in which case, independen
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Cosmology (in accord with the unive
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Cosmology (in accord with the unive
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Cosmology missing part making Ω =
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Cosmology missing part making Ω =
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Cosmology Appendix: Λ 0 The issue
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Cosmology physical effect of a non-
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Cosmology and the metric ds 2 = 1
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Cosmology and the metric ds 2 = 1
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Cosmology With a 2 1 K = 3 Λ ; a
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Cosmology With a 2 1 K = 3 Λ ; a
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Cosmology Λ < 0: Anti-de Sitter sp
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Cosmology Λ < 0: Anti-de Sitter sp
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Cosmology Note: z = constant is the