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Particle Physics and Cosmology Inflation
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Friedman Universe : horizon grows with time
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flatness problem
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Ω=1 : unstable fixed point
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inflationary kinematics
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exponential inflation
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end of inflation when ν gets < 1
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e - foldings
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inflationary cosmology with scalar field inflationary cosmology with scalar field
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energy density and pressure crucial ingredient : shape of scalar potential V
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field equations
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flat region in potential change of scalar is small effect, V,H essentially constant
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slow roll parameters
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single field inflation if
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slow roll approximation
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ν ≈ - ε
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chaotic inflation
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slow roll condition
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scales of fluctuations first out last in
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e - foldings
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