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Title: Flux flattening in axion monodromy inflation

Abstract

String theory models of axion monodromy inflation exhibit scalar potentials which are quadratic for small values of the inflaton field and evolve to a more complicated function for large field values. Oftentimes the large field behaviour is gentler than quadratic, lowering the tensor-to-scalar ratio. This effect, known as flattening, has been observed in the string theory context through the properties of the DBI+CS D-brane action. We revisit such flattening effects in type IIB flux compactifications with mobile D7-branes, with the inflaton identified with the D7-brane position. We observe that here, with a generic choice of background fluxes, flattening effects are larger than previously observed, allowing to fit these models within current experimental bounds. In particular, we compute the cosmological observables in scenarios compatible with closed-string moduli stabilisation, finding tensor-to-scalar ratios as low as r ~ 0.04. These are models of single field inflation in which the inflaton is much lighter than the other scalars through a mild tuning of the compactification data.

Authors:
 [1];  [1];  [2];  [2]
  1. Inst.de Física Teórica, Madrid (Spain)
  2. Univ. of Wisconsin, Madison, WI (United States). Dept. of Physics; Hong Kong Univ. of Science and Technology, Hong Kong (China). Inst. for Advanced Study
Publication Date:
Research Org.:
Univ. of Wisconsin, Madison, WI (United States)
Sponsoring Org.:
USDOE Office of Science (SC)
OSTI Identifier:
1533251
Grant/Contract Number:  
FG02-95ER40896
Resource Type:
Accepted Manuscript
Journal Name:
Journal of High Energy Physics (Online)
Additional Journal Information:
Journal Name: Journal of High Energy Physics (Online); Journal Volume: 2017; Journal Issue: 6; Journal ID: ISSN 1029-8479
Publisher:
Springer Berlin
Country of Publication:
United States
Language:
English
Subject:
physics; D-branes; flux compactifications; Cosmology of Theories beyond the SM; compactification and String Models

Citation Formats

Landete, Aitor, Marchesano, Fernando, Shiu, Gary, and Zoccarato, Gianluca. Flux flattening in axion monodromy inflation. United States: N. p., 2017. Web. doi:10.1007/jhep06(2017)071.
Landete, Aitor, Marchesano, Fernando, Shiu, Gary, & Zoccarato, Gianluca. Flux flattening in axion monodromy inflation. United States. doi:10.1007/jhep06(2017)071.
Landete, Aitor, Marchesano, Fernando, Shiu, Gary, and Zoccarato, Gianluca. Tue . "Flux flattening in axion monodromy inflation". United States. doi:10.1007/jhep06(2017)071. https://www.osti.gov/servlets/purl/1533251.
@article{osti_1533251,
title = {Flux flattening in axion monodromy inflation},
author = {Landete, Aitor and Marchesano, Fernando and Shiu, Gary and Zoccarato, Gianluca},
abstractNote = {String theory models of axion monodromy inflation exhibit scalar potentials which are quadratic for small values of the inflaton field and evolve to a more complicated function for large field values. Oftentimes the large field behaviour is gentler than quadratic, lowering the tensor-to-scalar ratio. This effect, known as flattening, has been observed in the string theory context through the properties of the DBI+CS D-brane action. We revisit such flattening effects in type IIB flux compactifications with mobile D7-branes, with the inflaton identified with the D7-brane position. We observe that here, with a generic choice of background fluxes, flattening effects are larger than previously observed, allowing to fit these models within current experimental bounds. In particular, we compute the cosmological observables in scenarios compatible with closed-string moduli stabilisation, finding tensor-to-scalar ratios as low as r ~ 0.04. These are models of single field inflation in which the inflaton is much lighter than the other scalars through a mild tuning of the compactification data.},
doi = {10.1007/jhep06(2017)071},
journal = {Journal of High Energy Physics (Online)},
number = 6,
volume = 2017,
place = {United States},
year = {2017},
month = {6}
}

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Cited by: 12 works
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