By Adnan Ghribi
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Additional info for Advances in Modern Cosmology
On this scenario we impose supergravity constraints, creating the NmSuGra model. Unsurprisingly though, testing a new theory for viability can pose a considerable challenge. Not only is it highly complex to calculate predictions for a given model, but invariably there will be degrees of freedom in the model which are not constrained by theoretical considerations, which must therefore become free parameters. Varying these creates a multiplicity of possibilities that can easily become unmanageable, and so sophisticated statistical techniques are required to keep track of supersymmetric predictions.
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It is now clear that for large positive y the vacuum energy in the ﬁrst term dominates and drives inﬂation until the vacuum energy is compensated by the y-dependent terms near ey = 1. 26 24 Advances in Modern Cosmology Will-be-set-by-IN-TECH It can be veriﬁed along the lines of ref. (33) that the formula for scalar perturbations remains 2 /(24π 2 M2 ), where N is the number of the same as that for the model (7), ie. Δ2R ≈ N 2 Minf Pl e-folds from the end of inﬂation. 5 · 1010 ( Ne /50)2 (140) Here the value of Δ R is taken from ref.
Advances in Modern Cosmology by Adnan Ghribi