Density matrix of the Universe and a new type of hill-top inflation

Andrei Barvinsky
Event Date and Time: 
Wed, 2016-10-05 12:00 - 13:00
Hennings 318
Local Contact: 
Philip Stamp
A widely accepted paradigm of inflationary scenario implies a quasi-vacuum state as an initial state of the Universe, its large scale structure eventually originating
from vacuum fluctuations of the quantum fields. We discuss the alternative scenario with the initial state of the Universe in the form of the microcanonical density matrix. Apart from advantages of aestatical and uniqueness nature this scenario, when applied to a cosmological model driven by a large number of conformal matter fields, provides us with a number of new interesting features. In particular, it restricts the range of the inflation energy scale (the effective cosmological constant) to the subplanckian domain, dynamically rules out the Hartle-Hawking no-boundary wavefunction and replaces it with the quasi-thermal state. This "some like it hot" scenario generates favorable initial conditions for a new type of hill-top inflation that could underlie the Higgs or Starobinsky $R^2$ inflation models.
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