Swampland Criteria of Inflationary Cosmology with Well-Known Potentials

Abstract

We explore the swampland conjectures of quintessence and tachyon scalar field models in f(T) and Einstein gravities, respectively. In f(T) gravity, we consider cold and warm (by assuming generalized dissipative coefficient) inflationary scenario and develop constraints on de-Sitter conjectures through Bekenstein entropy relation. In usual inflation, the deSitter conjecture constraint becomes constant (in terms of models constant parameters) which can be easily analyzed for its validity (i.e., |V0| V ≤O(1)). However, in warm inflation, we analyze the de-Sitter conjecture constraint through T0V TV0, i.e., if T0V TV0 < 1 then |V0| V ≤ O(1) and hence we can obtain required result. For evaluating this condition, we choose three well-known potentials such as monomial chaotic, hilltop and generalized exponential. It is observed that the condition T0V TV0 < 1 satisfied for all three potentials in both regimes of dissipative coefficient for specific choice of constants. Similarly, we also obtain satisfactory results of de-Sitter conjecture for tachyon and polytropic (with quintessence scalar field) in general relativity.