Inflation and the Theory of Cosmological Perturbations
Inflation and the Theory of Cosmological Perturbations A. Riotto INFN, Sezione di Padova, via Marzolo 8, I-35131, Padova, Italy. Abstract These lectures provide a pedagogical introduction to inflation and the theory of cosmological per- turbations generated during inflation which are thought to be the origin of structure in the universe. Lectures given at the: Summer School on arXiv:hep-ph/0210162v2 30 Jan 2017 Astroparticle Physics and Cosmology Trieste, 17 June - 5 July 2002 1 Notation A few words on the metric notation. We will be using the convention (−; +; +; +), even though we might switch time to time to the other option (+; −; −; −). This might happen for our convenience, but also for pedagogical reasons. Students should not be shielded too much against the phenomenon of changes of convention and notation in books and articles. Units We will adopt natural, or high energy physics, units. There is only one fundamental dimension, energy, after setting ~ = c = kb = 1, [Energy] = [Mass] = [Temperature] = [Length]−1 = [Time]−1 : The most common conversion factors and quantities we will make use of are 1 GeV−1 = 1:97 × 10−14 cm=6:59 × 10−25 sec, 1 Mpc= 3.08×1024 cm=1.56×1038 GeV−1, 19 MPl = 1:22 × 10 GeV, −1 −1 −42 H0= 100 h Km sec Mpc =2.1 h × 10 GeV, 2 −29 −3 2 4 −3 2 −47 4 ρc = 1:87h · 10 g cm = 1:05h · 10 eV cm = 8:1h × 10 GeV , −13 T0 = 2:75 K=2.3×10 GeV, 2 Teq = 5:5(Ω0h ) eV, Tls = 0:26 (T0=2:75 K) eV.
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