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Trapped quintessential inflation in the context of flux compactifications.

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Trapped quintessential inflation in the context of flux compactifications. / Bueno-Sanchez, Juan Carlos; Dimopoulos, Konstantinos.
In: Journal of Cosmology and Astroparticle Physics, Vol. 2007, No. 10, 04.10.2007, p. 002.

Research output: Contribution to Journal/MagazineJournal articlepeer-review

Harvard

Bueno-Sanchez, JC & Dimopoulos, K 2007, 'Trapped quintessential inflation in the context of flux compactifications.', Journal of Cosmology and Astroparticle Physics, vol. 2007, no. 10, pp. 002. https://doi.org/10.1088/1475-7516/2007/10/002

APA

Bueno-Sanchez, J. C., & Dimopoulos, K. (2007). Trapped quintessential inflation in the context of flux compactifications. Journal of Cosmology and Astroparticle Physics, 2007(10), 002. https://doi.org/10.1088/1475-7516/2007/10/002

Vancouver

Bueno-Sanchez JC, Dimopoulos K. Trapped quintessential inflation in the context of flux compactifications. Journal of Cosmology and Astroparticle Physics. 2007 Oct 4;2007(10):002. doi: 10.1088/1475-7516/2007/10/002

Author

Bueno-Sanchez, Juan Carlos ; Dimopoulos, Konstantinos. / Trapped quintessential inflation in the context of flux compactifications. In: Journal of Cosmology and Astroparticle Physics. 2007 ; Vol. 2007, No. 10. pp. 002.

Bibtex

@article{51725c90acd049448b6883d02b64aaf5,
title = "Trapped quintessential inflation in the context of flux compactifications.",
abstract = "We present a model for quintessential inflation using a string modulus for the inflaton–quintessence field. The scalar potential of our model is based on generic non-perturbative potentials arising in flux compactifications. We assume an enhanced symmetry point (ESP), which fixes the initial conditions for slow roll inflation. When crossing the ESP the modulus becomes temporarily trapped, which leads to a brief stage of trapped inflation. This is followed by enough slow roll inflation to solve the flatness and horizon problems. After inflation, the field rolls down the potential and eventually freezes to a certain value because of cosmological friction. The latter is due to the thermal bath of the hot big bang, which is produced by the decay of a curvaton field. The modulus remains frozen until the present, when it becomes quintessence.",
author = "Bueno-Sanchez, {Juan Carlos} and Konstantinos Dimopoulos",
year = "2007",
month = oct,
day = "4",
doi = "10.1088/1475-7516/2007/10/002",
language = "English",
volume = "2007",
pages = "002",
journal = "Journal of Cosmology and Astroparticle Physics",
issn = "1475-7516",
publisher = "IOP Publishing",
number = "10",

}

RIS

TY - JOUR

T1 - Trapped quintessential inflation in the context of flux compactifications.

AU - Bueno-Sanchez, Juan Carlos

AU - Dimopoulos, Konstantinos

PY - 2007/10/4

Y1 - 2007/10/4

N2 - We present a model for quintessential inflation using a string modulus for the inflaton–quintessence field. The scalar potential of our model is based on generic non-perturbative potentials arising in flux compactifications. We assume an enhanced symmetry point (ESP), which fixes the initial conditions for slow roll inflation. When crossing the ESP the modulus becomes temporarily trapped, which leads to a brief stage of trapped inflation. This is followed by enough slow roll inflation to solve the flatness and horizon problems. After inflation, the field rolls down the potential and eventually freezes to a certain value because of cosmological friction. The latter is due to the thermal bath of the hot big bang, which is produced by the decay of a curvaton field. The modulus remains frozen until the present, when it becomes quintessence.

AB - We present a model for quintessential inflation using a string modulus for the inflaton–quintessence field. The scalar potential of our model is based on generic non-perturbative potentials arising in flux compactifications. We assume an enhanced symmetry point (ESP), which fixes the initial conditions for slow roll inflation. When crossing the ESP the modulus becomes temporarily trapped, which leads to a brief stage of trapped inflation. This is followed by enough slow roll inflation to solve the flatness and horizon problems. After inflation, the field rolls down the potential and eventually freezes to a certain value because of cosmological friction. The latter is due to the thermal bath of the hot big bang, which is produced by the decay of a curvaton field. The modulus remains frozen until the present, when it becomes quintessence.

U2 - 10.1088/1475-7516/2007/10/002

DO - 10.1088/1475-7516/2007/10/002

M3 - Journal article

VL - 2007

SP - 002

JO - Journal of Cosmology and Astroparticle Physics

JF - Journal of Cosmology and Astroparticle Physics

SN - 1475-7516

IS - 10

ER -