Figure 8: The evolution of the covariant
variable , defined in
Equation (298)
(and not to be confused with the
Bardeen potential), along a fundamental world-line. This is a mode
that is well beyond the Hubble horizon
at , about 50 e-folds
before inflation ends, and remains super-Hubble through the radiation era. A smooth
transition from inflation to radiation is modelled by , where
is a small positive parameter
(chosen as in the
plot). Labels on the curves indicate the value of , so that the general
relativistic solution is the dashed
curve ( ).
(Figure taken from [122].)
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