3.1. The definition of inflation
Inflation is defined to be any epoch during which the Universe is accelerating, > 0, with respect to cosmic time. We can rewrite this in several different ways
The second of these is the most useful, because it has the most direct
geometrical interpretation. It says that the Hubble length, as
measured in comoving coordinates, decreases during inflation. At
any other time, the comoving Hubble length increases. This is the key
property of inflation; although typically the expansion of the
Universe is very rapid, the crucial characteristic scale of the
Universe is actually becoming smaller, when measured relative to that
expansion.
Quite a wide range of behaviours satisfy the inflationary
condition. The classic one is de Sitter expansion, which arises when
the Universe is dominated by a cosmological constant, which we saw
earlier gives
a(t)
exp(Ht). However realistic
models of inflation usually deviate from this idealized situation,
since inflation must come to an end to allow the successes of the
standard Hot Big Bang to be reproduced after one second or so.