Abstract:
In this thesis, our aim is to study cosmic warm inflation (WI) in the framework
of f(Q) gravity, where Q represents the non-metricity scalar. In this context,
we introduce the Tsallis, Renyi, and Barrow holographic dark energy (BHDE)
entropies into the standard Friedmann equations. Under the slow-roll (SR) ap-
proximation, we find exact solutions for the inflaton field, the effective potential
necessary to produce inflation, and the scale factor while considering both low
and high-dissipative regimes. We calculate some important parameters, includ-
ing SR parameters, the number of e-folds (N), the scalar spectral index (nS) and
its running (αs), and finally tensor-to-scalar ratio (r) for each model, in order
to assess the accuracy of the selected DE models in the light of observational
data. The ranges of the free parameters are derived from the limits on inflation-
ary observables imposed by Planck data. The obtained results remain within 2σ
confidence level and are consistent with physical predictions.
