A Spinodal Solution to Swampland Inflationary Constraints. (arXiv:1811.06021v1 [hep-th])
<a href="http://arxiv.org/find/hep-th/1/au:+Holman_R/0/1/0/all/0/1">R. Holman</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Richard_B/0/1/0/all/0/1">B. Richard</a>
We show how the inclusion of non-perturbative, {em dynamical} quantum
effects on the evolution of the inflaton can allow for an inflationary phase
that is both consistent with cosmological constraints {em and} avoids the
problems associated with the so-called swampland conditions. In particular, for
concave potentials such as those preferred by the Planck data, spinodal
instabilities associated with tachyonic masses for long wavelength modes induce
a second round of inflation, which in essence decouples the tree-level
potential from the inflationary phase. We illustrate these points using natural
inflation as an example.
We show how the inclusion of non-perturbative, {em dynamical} quantum
effects on the evolution of the inflaton can allow for an inflationary phase
that is both consistent with cosmological constraints {em and} avoids the
problems associated with the so-called swampland conditions. In particular, for
concave potentials such as those preferred by the Planck data, spinodal
instabilities associated with tachyonic masses for long wavelength modes induce
a second round of inflation, which in essence decouples the tree-level
potential from the inflationary phase. We illustrate these points using natural
inflation as an example.
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