Particle Physics and Cosmology Inflation

Friedman Universe : horizon grows with time

flatness problem

Ω=1 : unstable fixed point

inflationary kinematics

exponential inflation

end of inflation when ν gets < 1

e - foldings

inflationary cosmology with scalar field inflationary cosmology with scalar field

energy density and pressure crucial ingredient : shape of scalar potential V

field equations

flat region in potential change of scalar is small effect, V,H essentially constant

slow roll parameters

single field inflation if

slow roll approximation

ν ≈ - ε

chaotic inflation

slow roll condition

scales of fluctuations first out last in

e - foldings