Abstract
The de Sitter constraint on the space of effective scalar field theories consistent with superstring theory provides a lower bound on the slope of the potential of a scalar field which dominates the evolution of the Universe, e.g., a hypothetical inflaton field. Whereas models of single scalar field inflation with a canonically normalized field do not obey this constraint, it has been claimed recently in the literature that models of warm inflation can be made compatible with it in the case of large dissipation. The de Sitter constraint is known to be derived from entropy considerations. Since warm inflation necessary involves entropy production, it becomes necessary to determine how this entropy production will affect the constraints imposed by the swampland conditions. Here, we generalize these entropy considerations to the case of warm inflation and show that the condition on the slope of the potential remains essentially unchanged and is, hence, robust even in the warm inflation dynamics. We are then able to conclude that models of warm inflation indeed can be made consistent with the swampland criteria.
Highlights
Swampland conjectures through entropy considerationsIn ref. [1] it was argued that the range of applicability of any low energy EFT which results after compactification to four spacetime dimensions of a ten-dimensional string theory is constrained
In ref. [23], a derivation of the de Sitter conjecture was proposed which combines the distance criterion with an entropy argument
The de Sitter constraint on the space of effective scalar field theories consistent with superstring theory provides a lower bound on the slope of the potential of a scalar field which dominates the evolution of the Universe, e.g., a hypothetical inflaton field
Summary
In ref. [1] it was argued that the range of applicability of any low energy EFT which results after compactification to four spacetime dimensions of a ten-dimensional string theory is constrained. The reason for this bound is that if the scalar field moves a distance larger than that given by eq (2.1), a tower of new string states becomes low mass and must be included in the low energy EFT. Where ∇ is the gradient in field space, c2 and c3 are universal and positive constants of order 1 and min(∇i∇jV ) is the minimum eigenvalue of the Hessian ∇i∇Vj in an orthonormal frame. This means that either the potential is sufficiently steep, or else sufficiently tachyonic. We will extend the above analysis to WI
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