Strengthening the de Sitter swampland conjecture in warm inflation
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Springer
Received: March 4, 2020 Accepted: July 22, 2020 Published: August 25, 2020
Robert Brandenberger,a Vahid Kamalia,b,c and Rudnei O. Ramosd a
Department of Physics, McGill University, Montreal, QC H3A 2T8, Canada b Department of Physics, Bu-Ali Sina (Avicenna) University, Hamedan 65178 016016, Iran c School of Physics, Institute for Research in Fundamental Sciences (IPM), Tehran 19538-33511, Iran d Departamento de Fisica Teorica, Universidade do Estado do Rio de Janeiro, Rio de Janeiro, RJ 20550-013, Brazil
E-mail: [email protected], [email protected], [email protected] 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. Keywords: Cosmology of Theories beyond the SM, Spacetime Singularities ArXiv ePrint: 2002.04925
c The Authors. Open Access, Article funded by SCOAP3 .
https://doi.org/10.1007/JHEP08(2020)127
JHEP08(2020)127
Strengthening the de Sitter swampland conjecture in warm inflation
Contents 1
2 Swampland conjectures through entropy considerations
2
3 Warm inflation and de Sitter conjecture
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4 Examples 4.1 Monomials chaotic inflation models 4.2 Hilltop type of inflation models 4.3 Generalized exponential type of inflation models
8 8 9 9
5 Conclusions
1
10
Introduction
In order to understand the early evolution of the Universe at the highest energy scales, a consistent embedding of the physical model of the early Universe in a quantum theory of gravity is required. The only currently known consistent quantum gravity theory which unifies all forces of nature is superstring theory. Superstring theory leads to tight constraints (the so-called swampland constraints) on the space of possible effective field theories (EFT) which can be applied to study the evolution of the Universe. In particular, scalar fields arising in an EFT have a string-theoretical origin, and the range of validity of such EFTs and the potentials for the scalar fields are constrained. At the moment, the constraints are not at the level of theorem
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