Cosmological solutions of the Einstein-Friedmann equations ...

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Cosmology claimed to represent the vacuum energy density. The ideal fluid tensor structure then requires the vacuum energy, now usually called dark energy to satisfy the exotic equation of state pΛ = −ρΛ . c○ 2009, F. Jegerlehner ≪❘ Lect. 7 ❘≫ 440
Cosmology claimed to represent the vacuum energy density. The ideal fluid tensor structure then requires the vacuum energy, now usually called dark energy to satisfy the exotic equation of state pΛ = −ρΛ . In the following we discuss the resulting set of Friedmann equations c○ 2009, F. Jegerlehner ≪❘ Lect. 7 ❘≫ 440
Page 1 and 2: Cosmology Cosmological solutions of
Page 3 and 4: Cosmology Cosmological solutions of
Page 5: Cosmology claimed to represent the
Page 9 and 10: 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 and 38: 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
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Cosmology Back to the non-flat geom
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Cosmology Back to the non-flat geom
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Cosmology in terms of the observabl
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Cosmology The conclusion of the abo
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Cosmology C) Radiation dominated: p
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Cosmology ❖ k = 0 : S (t) = 4 ¯
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Cosmology In each case we have S (t
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Cosmology κ ρ(t) = 3 H2 (t) K(t)
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Cosmology Actually, in the radiatio
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Cosmology Actually, in the radiatio
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Cosmology 8π hν ργ(ν) dν = 3
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Cosmology 8π hν ργ(ν) dν = 3
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Cosmology Since ρ(t)S (t) 4 = ρ0S
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Cosmology c○ 2009, F. Jegerlehner
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Cosmology and Dicke and Peebles at
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Cosmology T0 = (2.725 ± 0.002) ◦
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Cosmology T0 = (2.725 ± 0.002) ◦
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Cosmology However, the evolution of
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Cosmology However, the evolution of
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Cosmology ρ(t) Big Bang radiation
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Cosmology The critical energy densi
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Cosmology Ω0 = 1 c○ 2009, F. Je
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Cosmology Ω0 = 1 is the critical
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Cosmology ˙S 2 c 2 + k = κ 3 ρ S
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Cosmology ˙S 2 c 2 + k = κ 3 ρ S
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Cosmology q0 = κ (ρ0+3 p0) 6 H 2
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Cosmology Form of energy equation o
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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
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