Tuesday, April 7, 2009, 3:30 pm — Large Seminar Room, Bldg. 510
Cosmic inflation is a hypothesized process in the early universe that generically explains a conundrum of cosmological puzzles: why is the universe spatially flat, isotropic and homogeneous, what gives rise to the primordial density fluctuations, why do these extend to scales larger than horizon and why do we not see topological defects. I will briefly explain the theory behind the cosmic inflation, its role as a unique window to the fundamental physics at very high energies and motivate four crucial cosmological observables that can help us distinguish between models of inflation and its alternatives. I will discuss the present observational status, our theoretical prejudices and the future of the field.
Hosted by: Morgan May
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