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The inflating curvaton

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The inflating curvaton. / Dimopoulos, Konstantinos; Kohri, Kazunori; Lyth, David; Matsuda, Tomohiro.

In: Journal of Cosmology and Astroparticle Physics, Vol. 03, JCAP03(2012)022, 12.03.2012, p. 0-8.

Research output: Contribution to journalJournal article

Harvard

Dimopoulos, K, Kohri, K, Lyth, D & Matsuda, T 2012, 'The inflating curvaton', Journal of Cosmology and Astroparticle Physics, vol. 03, JCAP03(2012)022, pp. 0-8. https://doi.org/10.1088/1475-7516/2012/03/022

APA

Dimopoulos, K., Kohri, K., Lyth, D., & Matsuda, T. (2012). The inflating curvaton. Journal of Cosmology and Astroparticle Physics, 03, 0-8. [JCAP03(2012)022]. https://doi.org/10.1088/1475-7516/2012/03/022

Vancouver

Dimopoulos K, Kohri K, Lyth D, Matsuda T. The inflating curvaton. Journal of Cosmology and Astroparticle Physics. 2012 Mar 12;03:0-8. JCAP03(2012)022. https://doi.org/10.1088/1475-7516/2012/03/022

Author

Dimopoulos, Konstantinos ; Kohri, Kazunori ; Lyth, David ; Matsuda, Tomohiro. / The inflating curvaton. In: Journal of Cosmology and Astroparticle Physics. 2012 ; Vol. 03. pp. 0-8.

Bibtex

@article{18d7fbbe80984befa2cc6f0ace68a6d2,
title = "The inflating curvaton",
abstract = "The primordial curvature perturbation zeta may be generated by some curvaton field sigma, which is negligible during inflation and has more or less negligible interactions until it decays. In the current scenario, the curvaton starts to oscillate while its energy density rho_sigma is negligible. We explore the opposite scenario, in which rho_sigma drives a few e-folds of inflation before the oscillation begins. In this scenario for generating zeta it is exceptionally easy to solve the eta-problem; one just has to make the curvaton a string axion, with anomaly-mediated susy breaking which may soon be tested at the LHC. The observed spectral index n can be obtained with a potential V~phi^p for the first inflation; p = 1 or 2 is allowed by the current uncertainty in n but the improvement in accuracy promised by Planck may rule out p = 1. The predictions include (i) running n'= 0.0026 (0.0013) for p = 1 (2) that will probably be observed, (ii) non-gaussianity parameter fNL ~ −1 that may be observed, (iii) tensor fraction r is probably too small to ever observed.",
author = "Konstantinos Dimopoulos and Kazunori Kohri and David Lyth and Tomohiro Matsuda",
year = "2012",
month = mar,
day = "12",
doi = "10.1088/1475-7516/2012/03/022",
language = "English",
volume = "03",
pages = "0--8",
journal = "Journal of Cosmology and Astroparticle Physics",
issn = "1475-7516",
publisher = "IOP Publishing",

}

RIS

TY - JOUR

T1 - The inflating curvaton

AU - Dimopoulos, Konstantinos

AU - Kohri, Kazunori

AU - Lyth, David

AU - Matsuda, Tomohiro

PY - 2012/3/12

Y1 - 2012/3/12

N2 - The primordial curvature perturbation zeta may be generated by some curvaton field sigma, which is negligible during inflation and has more or less negligible interactions until it decays. In the current scenario, the curvaton starts to oscillate while its energy density rho_sigma is negligible. We explore the opposite scenario, in which rho_sigma drives a few e-folds of inflation before the oscillation begins. In this scenario for generating zeta it is exceptionally easy to solve the eta-problem; one just has to make the curvaton a string axion, with anomaly-mediated susy breaking which may soon be tested at the LHC. The observed spectral index n can be obtained with a potential V~phi^p for the first inflation; p = 1 or 2 is allowed by the current uncertainty in n but the improvement in accuracy promised by Planck may rule out p = 1. The predictions include (i) running n'= 0.0026 (0.0013) for p = 1 (2) that will probably be observed, (ii) non-gaussianity parameter fNL ~ −1 that may be observed, (iii) tensor fraction r is probably too small to ever observed.

AB - The primordial curvature perturbation zeta may be generated by some curvaton field sigma, which is negligible during inflation and has more or less negligible interactions until it decays. In the current scenario, the curvaton starts to oscillate while its energy density rho_sigma is negligible. We explore the opposite scenario, in which rho_sigma drives a few e-folds of inflation before the oscillation begins. In this scenario for generating zeta it is exceptionally easy to solve the eta-problem; one just has to make the curvaton a string axion, with anomaly-mediated susy breaking which may soon be tested at the LHC. The observed spectral index n can be obtained with a potential V~phi^p for the first inflation; p = 1 or 2 is allowed by the current uncertainty in n but the improvement in accuracy promised by Planck may rule out p = 1. The predictions include (i) running n'= 0.0026 (0.0013) for p = 1 (2) that will probably be observed, (ii) non-gaussianity parameter fNL ~ −1 that may be observed, (iii) tensor fraction r is probably too small to ever observed.

U2 - 10.1088/1475-7516/2012/03/022

DO - 10.1088/1475-7516/2012/03/022

M3 - Journal article

VL - 03

SP - 0

EP - 8

JO - Journal of Cosmology and Astroparticle Physics

JF - Journal of Cosmology and Astroparticle Physics

SN - 1475-7516

M1 - JCAP03(2012)022

ER -