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I'm trying to get an overview of cosmological models which include inflation. My aim is to study the numerics of nonlinear Klein- Gordon equations which in fact are the Friedmann equations in the FRLW metric. \begin{equation} \ddot{\phi}+3 \dot{\phi} H + V'(\phi) =0. \end{equation}

Here $H$ stands for the Hubble constant and $\phi$ is representing the inflation field. I know there are several anstatzes for the inflation, especially I'm interested in the different potentials $V$ which occur in different models and why they are chosen this way (just a rough argument).

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  • $\begingroup$ A little dated, but this paper includes many of the popular phenomenological models: arxiv.org/abs/astro-ph/0510441 $\endgroup$ – bapowell Jul 6 '18 at 23:53
  • $\begingroup$ Forms of the potential are generally chosen because they reproduce observations (and vice versa, potentials have been ruled out because they make non-physical predictions). $\endgroup$ – astronat Jul 7 '18 at 21:23

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