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  • 1706.09735

    Rights statement: This is the author’s version of a work that was accepted for publication in Astroparticle Physics. Changes resulting from the publishing process, such as peer review, editing, corrections, structural formatting, and other quality control mechanisms may not be reflected in this document. Changes may have been made to this work since it was submitted for publication. A definitive version was subsequently published in Astroparticle Physics, 103, 2018 DOI: 10.1016/j.astropartphys.2018.06.002

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Loop inflection-point inflation

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Loop inflection-point inflation. / Dimopoulos, Konstantinos; Owen, Charlotte; Racioppi, Antonio.
In: Astroparticle Physics, Vol. 103, 12.2018, p. 16-20.

Research output: Contribution to Journal/Magazine › Journal article › peer-review

Harvard

Dimopoulos, K, Owen, C & Racioppi, A 2018, 'Loop inflection-point inflation', Astroparticle Physics, vol. 103, pp. 16-20. https://doi.org/10.1016/j.astropartphys.2018.06.002

APA

Dimopoulos, K., Owen, C., & Racioppi, A. (2018). Loop inflection-point inflation. Astroparticle Physics, 103, 16-20. https://doi.org/10.1016/j.astropartphys.2018.06.002

Vancouver

Dimopoulos K, Owen C, Racioppi A. Loop inflection-point inflation. Astroparticle Physics. 2018 Dec;103:16-20. Epub 2018 Jun 14. doi: 10.1016/j.astropartphys.2018.06.002

Author

Dimopoulos, Konstantinos ; Owen, Charlotte ; Racioppi, Antonio. / Loop inflection-point inflation. In: Astroparticle Physics. 2018 ; Vol. 103. pp. 16-20.

Bibtex

@article{15883d0f75564e9f83d7135396042090,
title = "Loop inflection-point inflation",
abstract = "A novel inflection-point inflation model is analysed. The model considers a massless scalar field, whose self-coupling{\textquoteright}s running is stabilised by a non-renormalisable operator. The running is controlled by a fermion loop. We find that successful inflation is possible for a natural value of the Yukawa coupling y≃4×10^{−4}. The necessary fine-tuning is only ∼10^{−6}, which improves on the typical tuning of inflection-point inflation models, such as MSSM inflation. The model predicts a spectral index within the 1-σ bound of the latest CMB observations, with a very small negative running, and negligible tensors (r∼10^{−(9−10)}). These results are largely independent of the order of the stabilising non-renormalisable operator.",
keywords = "cosmic inflation, particle phenomenology",
author = "Konstantinos Dimopoulos and Charlotte Owen and Antonio Racioppi",
note = "This is the author{\textquoteright}s version of a work that was accepted for publication in Astroparticle Physics. Changes resulting from the publishing process, such as peer review, editing, corrections, structural formatting, and other quality control mechanisms may not be reflected in this document. Changes may have been made to this work since it was submitted for publication. A definitive version was subsequently published in Astroparticle Physics, 103, 2018 DOI: 10.1016/j.astropartphys.2018.06.002",
year = "2018",
month = dec,
doi = "10.1016/j.astropartphys.2018.06.002",
language = "English",
volume = "103",
pages = "16--20",
journal = "Astroparticle Physics",
issn = "0927-6505",
publisher = "Elsevier",

}

RIS

TY - JOUR

T1 - Loop inflection-point inflation

AU - Dimopoulos, Konstantinos

AU - Owen, Charlotte

AU - Racioppi, Antonio

N1 - This is the author’s version of a work that was accepted for publication in Astroparticle Physics. Changes resulting from the publishing process, such as peer review, editing, corrections, structural formatting, and other quality control mechanisms may not be reflected in this document. Changes may have been made to this work since it was submitted for publication. A definitive version was subsequently published in Astroparticle Physics, 103, 2018 DOI: 10.1016/j.astropartphys.2018.06.002

PY - 2018/12

Y1 - 2018/12

N2 - A novel inflection-point inflation model is analysed. The model considers a massless scalar field, whose self-coupling’s running is stabilised by a non-renormalisable operator. The running is controlled by a fermion loop. We find that successful inflation is possible for a natural value of the Yukawa coupling y≃4×10^{−4}. The necessary fine-tuning is only ∼10^{−6}, which improves on the typical tuning of inflection-point inflation models, such as MSSM inflation. The model predicts a spectral index within the 1-σ bound of the latest CMB observations, with a very small negative running, and negligible tensors (r∼10^{−(9−10)}). These results are largely independent of the order of the stabilising non-renormalisable operator.

AB - A novel inflection-point inflation model is analysed. The model considers a massless scalar field, whose self-coupling’s running is stabilised by a non-renormalisable operator. The running is controlled by a fermion loop. We find that successful inflation is possible for a natural value of the Yukawa coupling y≃4×10^{−4}. The necessary fine-tuning is only ∼10^{−6}, which improves on the typical tuning of inflection-point inflation models, such as MSSM inflation. The model predicts a spectral index within the 1-σ bound of the latest CMB observations, with a very small negative running, and negligible tensors (r∼10^{−(9−10)}). These results are largely independent of the order of the stabilising non-renormalisable operator.

KW - cosmic inflation

KW - particle phenomenology

U2 - 10.1016/j.astropartphys.2018.06.002

DO - 10.1016/j.astropartphys.2018.06.002

M3 - Journal article

VL - 103

SP - 16

EP - 20

JO - Astroparticle Physics

JF - Astroparticle Physics

SN - 0927-6505

ER -