Study of warm inflationary models and their parameter estimation from CMB. (arXiv:1812.03107v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Arya_R/0/1/0/all/0/1">Richa Arya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rangarajan_R/0/1/0/all/0/1">Raghavan Rangarajan</a>
Observations of the temperature anisotropies in the Cosmic Microwave
Background (CMB) radiation show that the models of inflation with the monomial
potentials are inconsistent with the allowed $n_s-r$ bounds. However certain
monomial potentials of inflation are allowed in the context of textit{Warm
Inflation}, where the inflaton’s coupling with other fields are significant
both textit{during and after} the inflationary phase. In our study, we
consider $lambdaphi^4$ and $lambdaphi^6$ models of warm inflation with
different forms of the inflaton dissipation coefficient. We parameterize the
primordial power spectrum in terms of the model parameters, namely, the
inflaton self coupling, $lambda$, and the dissipation parameter, $Q_P$, due to
inflaton’s interaction with the other fields. Then we obtain the joint and
marginal distributions of these parameters by carrying out a Markov Chain Monte
Carlo (MCMC) analysis using the {tt CosmoMC} numerical code. An estimation of
these physical parameters is essential for model building. We also obtain the
$n_s$ and $r$ values for the mean values of the parameters and find them to be
consistent with the observational bounds, confirming that these simple models
are viable models for describing inflation.
Observations of the temperature anisotropies in the Cosmic Microwave
Background (CMB) radiation show that the models of inflation with the monomial
potentials are inconsistent with the allowed $n_s-r$ bounds. However certain
monomial potentials of inflation are allowed in the context of textit{Warm
Inflation}, where the inflaton’s coupling with other fields are significant
both textit{during and after} the inflationary phase. In our study, we
consider $lambdaphi^4$ and $lambdaphi^6$ models of warm inflation with
different forms of the inflaton dissipation coefficient. We parameterize the
primordial power spectrum in terms of the model parameters, namely, the
inflaton self coupling, $lambda$, and the dissipation parameter, $Q_P$, due to
inflaton’s interaction with the other fields. Then we obtain the joint and
marginal distributions of these parameters by carrying out a Markov Chain Monte
Carlo (MCMC) analysis using the {tt CosmoMC} numerical code. An estimation of
these physical parameters is essential for model building. We also obtain the
$n_s$ and $r$ values for the mean values of the parameters and find them to be
consistent with the observational bounds, confirming that these simple models
are viable models for describing inflation.
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