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SUMMARY:Cosmology of f(R) gravity - Alexei Starobinsky (Landau Institute)
DTSTART:20100208T130000Z
DTEND:20100208T140000Z
UID:TALK22676@talks.cam.ac.uk
CONTACT:Tasos Avgoustidis
DESCRIPTION:Since 1980\, a variant of the f(R) fourth-order theory of grav
 ity (with small one-loop corrections) was known to provide an internally s
 elf-consistent scenario of the early Universe with an initial quasi-de Sit
 ter (inflationary) stage followed by the graceful exit to the radiation-do
 minated FRW stage via the period\nof reheating in which all matter in the 
 Universe arises as a result of gravitational particle creation. Its predic
 tions regarding spectra of primordial density perturbations and gravitatio
 nal waves remain in agreement with the most recent observational data. A f
 ew years ago it was proposed to use this class of models for description o
 f dark energy in the present Universe. However\, this problem appeared to 
 be more complicated\,\nso many attempts in this direction failed. Still re
 cently some f(R) models of dark energy have been found which can satisfy l
 aboratory\, Solar system and cosmological tests. To avoid formation of add
 itional singularities\, viable f(R) models of present dark energy should h
 ave the same asymptotic behaviour for large R as f(R) models of inflation.
  Unified description of inflation and present dark energy in f(R) gravity 
 is possible\, but leads to completely different reheating after inflation 
 during which strongly non-linear oscillations of R occur.
LOCATION:CMS\, Pav.B\, CTC Common Room (B1.19)
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