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Astronomy · L5 · Cosmic Inflation: Solving the Horizon and Flatness Problems · flowchart

Astronomy
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Inflaton field φin a flat region of V(φ)Slow roll:kinetic energy ≪ V(φ)Quasi-exponential expansiona(t) ∝ e^{Ht}, N ≳ 60Horizon problem solved:causal patch stretched beyondthe observable universeFlatness problem solved:curvature radius stretched,Ω driven toward 1φ reaches steep partof potentialInflation endsφ oscillates about V minimumReheating:inflaton energy decays intoStandard Model particlesHot, dense radiation-dominateduniverse — the standard Big Bang resumes
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