Swampland criteria and constraints on inflation in a f(R,T) gravity theory

Abstract

In this paper, we worked in the framework of an inflationary [Formula: see text] theory in the presence of a canonical scalar field. More specifically, the [Formula: see text] gravity. The values of the dimensionless parameters [Formula: see text] and [Formula: see text] are taken to be [Formula: see text] and [Formula: see text]. The motivation for this study was the striking similarities between the slow-roll parameters of the inflationary model used in this work and the ones obtained by the rescaled Einstein–Hilbert gravity inflation [Formula: see text]. We examined a variety of potentials to determine if they agree with the current Planck Constraints. In addition, we checked whether these models satisfy the Swampland Criteria and we specified the exact region of the parameter space that produces viable results for each model. As we mention in Sec. 4, the inflationary [Formula: see text] theory used in this work cannot produce a positive [Formula: see text] which implies that the stochastic gravitational wave background will not be detectable.

Constant-roll inflation with tachyon field in the holographic braneworld

“…From the swampland criteria, it may be seen that the range traversed by the field is bounded from above, and there is a lower bound on the gradient of the potential. As pointed out in [46,47], the swampland conjectures will be met if at least one of the conditions is satisfied. In the following, we will examine whether the second criterion (82) is satisfied in our model.…”

Are f(R, Matter) theories really relevant to cosmology?

“…This approach has been used to claim that f (R, Matter) gravity can explain various cosmological and astrophysical observations. In the context of cosmology, those applications range from inflation [14][15][16][17][18][19] to dark matter [20][21][22] and dark energy [23][24][25].…”