Figure 8: The evolution of the covariant variable , defined in Equation (304) (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 [177].)
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