Home > Research > Publications & Outputs > The TeV-mass curvaton
View graph of relations

The TeV-mass curvaton

Research output: Contribution to Journal/MagazineJournal articlepeer-review

Published

Standard

The TeV-mass curvaton. / Enqvist, Kari; Mazumdar, Anupam; Taanila, Olli.
In: Journal of Cosmology and Astroparticle Physics, Vol. 2010, No. 9, 30, 27.09.2010.

Research output: Contribution to Journal/MagazineJournal articlepeer-review

Harvard

Enqvist, K, Mazumdar, A & Taanila, O 2010, 'The TeV-mass curvaton', Journal of Cosmology and Astroparticle Physics, vol. 2010, no. 9, 30. https://doi.org/10.1088/1475-7516/2010/09/030

APA

Enqvist, K., Mazumdar, A., & Taanila, O. (2010). The TeV-mass curvaton. Journal of Cosmology and Astroparticle Physics, 2010(9), Article 30. https://doi.org/10.1088/1475-7516/2010/09/030

Vancouver

Enqvist K, Mazumdar A, Taanila O. The TeV-mass curvaton. Journal of Cosmology and Astroparticle Physics. 2010 Sept 27;2010(9):30. doi: 10.1088/1475-7516/2010/09/030

Author

Enqvist, Kari ; Mazumdar, Anupam ; Taanila, Olli. / The TeV-mass curvaton. In: Journal of Cosmology and Astroparticle Physics. 2010 ; Vol. 2010, No. 9.

Bibtex

@article{989a5685e9a040c4ae99b29678d54403,
title = "The TeV-mass curvaton",
abstract = "We consider the constraints for a curvaton with mass m ~ 1 TeV and show that they are not consistent with a purely quadratic potential. Even if the curvaton self-interactions were very weak, they must be accounted for as they affect the dynamical evolution of the curvature perturbation. We show that the only TeV-mass curvaton interaction potential that yields the correct perturbation amplitude, decays before the dark matter freeze-out, and does not give rise to non-Gaussian perturbations that are in conflict with the present limits, is given by V_int= sigma^8/M^4. The decay width of the curvaton should be in the range Gamma= 10^-15...10^-17 GeV. The model typically predicts large non-linearity parameters f_NL and g_NL that should be observable by the Planck satellite. We also discuss various physical possibilities to obtain the required small curvaton decay rate.",
keywords = "inflation , physics of the early universe",
author = "Kari Enqvist and Anupam Mazumdar and Olli Taanila",
year = "2010",
month = sep,
day = "27",
doi = "10.1088/1475-7516/2010/09/030",
language = "English",
volume = "2010",
journal = "Journal of Cosmology and Astroparticle Physics",
issn = "1475-7516",
publisher = "IOP Publishing",
number = "9",

}

RIS

TY - JOUR

T1 - The TeV-mass curvaton

AU - Enqvist, Kari

AU - Mazumdar, Anupam

AU - Taanila, Olli

PY - 2010/9/27

Y1 - 2010/9/27

N2 - We consider the constraints for a curvaton with mass m ~ 1 TeV and show that they are not consistent with a purely quadratic potential. Even if the curvaton self-interactions were very weak, they must be accounted for as they affect the dynamical evolution of the curvature perturbation. We show that the only TeV-mass curvaton interaction potential that yields the correct perturbation amplitude, decays before the dark matter freeze-out, and does not give rise to non-Gaussian perturbations that are in conflict with the present limits, is given by V_int= sigma^8/M^4. The decay width of the curvaton should be in the range Gamma= 10^-15...10^-17 GeV. The model typically predicts large non-linearity parameters f_NL and g_NL that should be observable by the Planck satellite. We also discuss various physical possibilities to obtain the required small curvaton decay rate.

AB - We consider the constraints for a curvaton with mass m ~ 1 TeV and show that they are not consistent with a purely quadratic potential. Even if the curvaton self-interactions were very weak, they must be accounted for as they affect the dynamical evolution of the curvature perturbation. We show that the only TeV-mass curvaton interaction potential that yields the correct perturbation amplitude, decays before the dark matter freeze-out, and does not give rise to non-Gaussian perturbations that are in conflict with the present limits, is given by V_int= sigma^8/M^4. The decay width of the curvaton should be in the range Gamma= 10^-15...10^-17 GeV. The model typically predicts large non-linearity parameters f_NL and g_NL that should be observable by the Planck satellite. We also discuss various physical possibilities to obtain the required small curvaton decay rate.

KW - inflation

KW - physics of the early universe

U2 - 10.1088/1475-7516/2010/09/030

DO - 10.1088/1475-7516/2010/09/030

M3 - Journal article

VL - 2010

JO - Journal of Cosmology and Astroparticle Physics

JF - Journal of Cosmology and Astroparticle Physics

SN - 1475-7516

IS - 9

M1 - 30

ER -