Fiber inflation and reheating

We present constraints on the reheating era within the string fiber inflation scenario, in terms of the effective equation-of-state parameter of the reheating fluid, w_reh . The results of the analysis, completely independent on the details of the inflaton physics around the vacuum, illustrate the behavior of the number of e -foldings during the reheating stage, N_reh, and of the final reheating temperature, T_reh, as functions of the scalar spectral index, n_s. We analyze our results with respect to the current bounds given by the Planck mission data and to upcoming cosmological experiments. We find that large values of the equation-of-state parameter (w_reh>1 /3 ) are particularly favored as the scalar spectral index is of the order of n_s∼0.9680 , with a σ_{n s}∼0.002 error. Moreover, we compare the behavior of the general reheating functions N_reh and T_reh in the fiber inflation scenario with the one extracted by the class of the α -attractor models with α =2 . We find that the corresponding reheating curves are very similar in the two cases.