By Daniel Baumann, Liam McAllister
ISBN-10: 1107089697
ISBN-13: 9781107089693
The earlier twenty years have visible transformative advances in cosmology and string idea. Observations of the cosmic microwave history have published powerful proof for inflationary growth within the very early universe, whereas new insights approximately compactifications of string thought have ended in a deeper realizing of inflation in a framework that unifies quantum mechanics and normal relativity. Written via of the major researchers within the box, this whole and obtainable quantity offers a latest therapy of inflationary cosmology and its connections to thread conception and user-friendly particle idea. After an up to date experimental precis, the authors current the rules of powerful box conception, string concept, and string compactifications, surroundings the degree for a close exam of versions of inflation in string thought. 3 appendices comprise historical past fabric in geometry and cosmological perturbation conception, making this a self-contained source for graduate scholars and researchers in string conception, cosmology, and comparable fields
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Extra resources for Inflation and string theory
Sample text
First of all, unlike the Stokes parameters, the parameters E and B are independent of the choice of coordinates. More importantly, symmetry forbids the generation of B-modes by scalar fluctuations [77, 78]. B-modes are therefore a crucial signature of the presence of tensor (or vector) fluctuations. 3 Large-scale structure The density perturbations are small at recombination, but under the influence of gravity they grow [79], eventually forming the large-scale structure of the universe. A linear order, the initial conditions from inflation are related to the dark matter density contrast δ ≡ δρ/ρ at redshift z via a transfer function Tδ (z, k), Pδ (z, k) = Tδ2 (z, k)PR (k) .
This implies that comoving scales (cs k) horizon at early times and re-enter the horizon at late times. In physical coor−1 dinates, the Hubble radius H is constant and the physical wavelength grows Ht exponentially, λ ∝ a(t) ∝ e . For adiabatic fluctuations, the curvature perturbations R do not evolve outside of the horizon, so the power spectrum PR (k) at horizon exit during inflation can be related directly to CMB observables at late times. ωk (t) ≡ cs k . 21) At early times (small a), ωk H for all modes of interest.
In single-field inflation, π is the unique fluctuation mode [51], while in multi-field inflation, additional light fields can contribute to R: see Appendix B. As we will see in Chapter 4, string theory strongly motivates considering scenarios in which multiple fields are light during inflation. However, from a purely bottom-up perspective, extra light fields during inflation are not required by present observations, and in this section we will focus on the minimal case of a single light field. One can learn a great deal about the CMB perturbations by studying the Goldstone boson fluctuations alone.
Inflation and string theory by Daniel Baumann, Liam McAllister
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