| Very Early Universe |
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| • | Inflation
(Guth, others, early 1980s) |
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| resolves
some of these properties. Inflation |
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| posits
an early exponential expansion of the |
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| universe
that leaves the curvature flat (close |
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| to
omega = 1) and takes regions in causal |
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| contact
and moves them far beyond their |
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| local
horizons (isotropy). May help form |
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| the
fluctuations leading to galaxies. |
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