Introduction to Cosmology

Consensus Inflation 161 Inhomogeneities of the energy density increase as the Universe develops from an ordered, homogeneous low ...

162 Cosmic Inflation As long as there were no decays or annihilations of massive particles, and all other interactions conserve ...

Consensus Inflation 163 S B 3 B 1 A 1 A 2 10 –^4310 –^351017 1030 10108 1 t[s] B 4 B 2 Figure 7.3Evolution of the scale푅of the U ...

164 Cosmic Inflation Perturbations. Density perturbations in the cosmological fluid of wavelength훬shift with the scale푎(푡)of the ...

The Chaotic Model 165 The metric perturbations can be decomposed into scalar, vector, and tensor pertur- bations, of which the v ...

166 Cosmic Inflation with퐻given by 퐻= 2 √ 휋 3 푚휙 푀P 휙푎. (7.48) At time휏, the Universe has expanded from a linear size푅(푡푎)to 푅(휏 ...

The Chaotic Model 167 fluctuations. This can be seen if one transforms the de Sitter metric (5.60) into the metric of a Euclidea ...

168 Cosmic Inflation continuously the volume of space grows by a factor e(^3 −ln 2)Ht, (7.56) whereas in the parts of space-time ...

A Cyclic Universe 169 Universe, we also have a precise theoretical specification for how much matter there should be. This links ...

170 Cosmic Inflation ordinary matter and radiation are created by oscillations in the potential well, or by entropy generation d ...

A Cyclic Universe 171 Early attempts to build models with cyclically reoccurring expansion and contrac- tion were plagued by the ...

172 Cosmic Inflation has decreased to the point where푉(휙)=^12 휙^2 where the field crosses zero potential, the total energy densi ...

A Cyclic Universe 173 scale of 10−^25 cm. In the cyclic Universe, the fluctuations can be generated a fraction of a second befor ...

174 Cosmic Inflation Show that the number of e-foldings of inflation in the푉(휙)=−휆휙^4 model is of order 푁≈퐻 2 휆휙^2 푖 fromtheti ...

8 Cosmic Microwave Background In this chapter we shall meet several important observational discoveries. The cosmic microwave ba ...

176 Cosmic Microwave Background 8.1 The CMB Temperature Predictions. In 1948,Georg Gamow(1904–1968),Ralph AlpherandRobert Herman ...

The CMB Temperature 177 To their consternation and annoyance they found a constant low level of back- ground noise in every dire ...

178 Cosmic Microwave Background Making use of Equations (6.10) and (8.5), the distribution at time푡′becomes d푛′훾(휈′)=^8 휋 3 푐^3 ...

The CMB Temperature 179 one steradian of sky. In SI units this is 10−^9 Jm−^1 sr−^1 s−^1. This quantity is equivalent to the int ...

180 Cosmic Microwave Background 8.2 Temperature Anisotropies Dipole Anisotropy. The temperature measurement of Penzias and Wilso ...