By Jérôme Gleyzes
This thesis offers a number of major new effects that make clear significant puzzles of contemporary cosmology: the character of inflation, the very early section of the universe that's inspiration to have given upward thrust to the large-scale buildings that we realize this day; and that of the present speeded up enlargement. particularly, it develops a fresh technique for characterizing linear cosmological perturbations for basic theories the place gravity is changed and/or plagued by a brand new part, referred to as darkish power, liable for the speeded up enlargement. It proposes a brand new extension to what have been lengthy considered the main common scalar box theories without instabilities, and demonstrates the robustness of the relation among the power scale of inflation and the anticipated amplitude of gravitational waves. eventually, it consolidates a suite of consistency family members among correlation features of the cosmological density box and investigates the phenomenological effects in their capability violation. awarded in a transparent, succinct and rigorous kind, each one of those unique effects is either profound and significant and may depart a deep mark at the field.
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Extra info for Dark Energy and the Formation of the Large Scale Structure of the Universe
81) we assumed the presence of a Jordan frame, where matter is minimally coupled, its stress energy tensor is conserved independently. 8 More precisely, to remove also the variable χ one needs a spatial diffeomorphism x i → x i + ∂ β. i 40 2 The Effective Field Theory of Dark Energy • The momentum constraint ((0i) components of Einstein’s equation) reads (ρm + pm )vm ρm + pm π =− . 83) • The trace of the same components gives, using the equation above, 2 ¨ + 2(3 + α M )H ˙ + 2(1 + α B )H ˙ ρm + pm + (α B H )· + (3 + α M )(1 + α B )H 2 + 2 H˙ − 2M 2 ρm + pm − 2H α B π¨ + 2 H˙ + − (α B H )· − (3 + α M )α B H 2 π˙ 2M 2 2 p˙ m ¨ π = 1 δpm − 2 k σm .
51) while all the others coefficients and φ˙ 0 is the background value of the scalar field. One can indeed check that CDM corresponds to all the αi being zero: one recovers the cosmological constant for φ˙ 0 = 0, which would set α K = 0. As a side note, it might seem odd that the potential V does not appear in Eq. 51). The reason is that this parametrization is specifically designed to look at linear perturbations, while V is a background quantity in unitary gauge. More precisely, the Friedmann equations impose V = 2 MPl 2 H˙ + 3H 2 (2 − 2 m) .
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Dark Energy and the Formation of the Large Scale Structure of the Universe by Jérôme Gleyzes