Warm inflationary model in loop quantum cosmology

A warm inflationary universe model in loop quantum cosmology is studied. In general we discuss the condition of inflation in this framework. By using a chaotic potential, $V(\varphi )\propto {\varphi }^2$, we develop a model where the dissipation coefficient $\Gamma ={\Gamma }_0=\mathrm{\text{constant}}$. We use recent astronomical observations for constraining the parameters appearing in our model.

Figure 1

The plot shows $r$ versus $n_s$ for two values of $m$. Here, we have fixed the values $T_r\simeq 0.24\times {10}^{16}\mathrm{GeV}$, ${\Gamma }_0\simeq 0.5\times {10}^{13}\mathrm{GeV}$, and ${\rho }_c\approx 0.82m_p^4$, respectively. The five-year WMAP data places stronger limits on the tensor-scalar ratio (shown in blue) than three-year data (grey) [35].