Cosmological solutions of the Einstein-Friedmann equations ...

More documents

Recommendations

Info

$Einführung in LaTeX - Www-com.physik.hu-berlin.de$

Cosmology ct = C arcsin √ X − √ X − X 2 ; X = S (t)/C Parameter representation: S (t) = 1 2 C (1 − cos η) 1 ct = 2 C (η − sin η) cycloid c○ 2009, F. Jegerlehner ≪❘ Lect. 7 ❘≫ 446
Cosmology ct = C arcsin √ X − √ X − X 2 ; X = S (t)/C Parameter representation: ❖ k = −1 : S (t) = 1 2 C (1 − cos η) 1 ct = 2 C (η − sin η) ct = C √ X + X 2 − arcsinh √ X ; X = S (t)/C cycloid c○ 2009, F. Jegerlehner ≪❘ Lect. 7 ❘≫ 446
Page 1 and 2: Cosmology Cosmological solutions of
Page 3 and 4: Cosmology Cosmological solutions of
Page 5 and 6: Cosmology claimed to represent the
Page 11 and 12: Cosmology A) Empty Worlds, vacuum e
Page 13 and 14: Cosmology A) Empty Worlds, vacuum e
Page 15 and 16: Cosmology The general solution is S
Page 21 and 22: Cosmology (d) Λ > 0 , k = 0: S = e
Page 27 and 28: Cosmology Terminology: Λ > 0 , k =
Page 33 and 34: Cosmology B) Matter dominated: ρ >
Page 35 and 36: Cosmology B) Matter dominated: ρ >
Page 37: 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 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
Page 69 and 70: Cosmology The conclusion of the abo
Page 75 and 76: Cosmology C) Radiation dominated: p
Page 81 and 82: Cosmology ❖ k = 0 : S (t) = 4 ¯
Page 89 and 90:
Cosmology κ ρ(t) = 3 H2 (t) K(t)
Page 91 and 92:
Cosmology Actually, in the radiatio
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
Page 103 and 104:
Cosmology and Dicke and Peebles at
Page 105 and 106:
Cosmology T0 = (2.725 ± 0.002) ◦
Page 107 and 108:
Cosmology T0 = (2.725 ± 0.002) ◦
Page 109 and 110:
Cosmology However, the evolution of
Page 111 and 112:
Cosmology However, the evolution of
Page 113 and 114:
Cosmology ρ(t) Big Bang radiation
Page 115 and 116:
Cosmology The critical energy densi
Page 117 and 118:
Page 119 and 120:
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:
Page 127 and 128:
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
Page 137 and 138:
Page 139 and 140:
Page 141 and 142:
Cosmology in which case, independen
Page 143 and 144:
Page 145 and 146:
Page 147 and 148:
Cosmology (in accord with the unive
Page 149 and 150:
Cosmology (in accord with the unive
Page 151 and 152:
Cosmology missing part making Ω =
Page 153 and 154:
Cosmology missing part making Ω =
Page 155 and 156:
Cosmology Appendix: Λ 0 The issue
Page 157 and 158:
Cosmology physical effect of a non-
Page 159 and 160:
Cosmology and the metric ds 2 = 1
Page 161 and 162:
Cosmology and the metric ds 2 = 1
Page 163 and 164:
Cosmology With a 2 1 K = 3 Λ ; a
Page 165 and 166:
Cosmology With a 2 1 K = 3 Λ ; a
Page 167 and 168:
Cosmology Λ < 0: Anti-de Sitter sp
Page 169 and 170:
Cosmology Λ < 0: Anti-de Sitter sp
Page 171 and 172:
Cosmology Note: z = constant is the
show all

Cosmological solutions of the Einstein-Friedmann equations ...

Create successful ePaper yourself

Delete template?

Save as template?