History of the Universe

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Presentation transcript:

History of the Universe How did the universe evolve so uniformly? Why is the CMBR temperature the same everywhere ? When and how did matter form ? Why are the H and He abundances the same everywhere (except for He produced in stars) ? Why is the expansion accelerating? Is the universe open or closed ?

The Big Bang Three basic facts based on observations: 1. Expansion of the Universe – Hubble Law 2. Cosmic Background Radiation 3. Primordial Nucleosynthesis : Cosmic abundances of H, He, and light elements

Primordial abundances of elements

Fluctuations and Large-Scale Structure Disturbances in the early universe grow in time; their size determines large-scale structure and properties such as the curvature of the universe.

“Hot spots” in the early universe as we see them today: Indicators of the curvature of the Universe

Uniformity and Isotropy of CMBR Why is the temperature of CMBR the same everywhere? The extremely uniform background radiation everywhere in the Universe presents a problem since different parts of the Universe may have been out of touch (even by light) from each other, i.e. outside each other’s event horizons

Observable Universe

Early to Present Universe (Flat?)

Temperature Evolution of the Universe

Temporal Evolution of the Universe

History of forces and particles in the Universe

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