Planck mass and inflation as consequences of dynamically broken scale invariance
Classical scale invariance represents a promising framework for model building beyond the Standard Model. However, once coupled to gravity, any scale-invariant microscopic model requires an explanation for the origin of the Planck mass. In this paper, we provide a minimal example for such a mechanis...
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| Hauptverfasser: | , , , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
23 July 2019
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| In: |
Physical review
Year: 2019, Jahrgang: 100, Heft: 1 |
| ISSN: | 2470-0029 |
| DOI: | 10.1103/PhysRevD.100.015037 |
| Online-Zugang: | Verlag, Volltext: https://doi.org/10.1103/PhysRevD.100.015037 Verlag: https://link.aps.org/doi/10.1103/PhysRevD.100.015037 
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| Verfasserangaben: | Jisuke Kubo, Manfred Lindner, Kai Schmitz, and Masatoshi Yamada |
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| 520 | |a Classical scale invariance represents a promising framework for model building beyond the Standard Model. However, once coupled to gravity, any scale-invariant microscopic model requires an explanation for the origin of the Planck mass. In this paper, we provide a minimal example for such a mechanism and show how the Planck mass can be dynamically generated in a strongly coupled gauge sector. We consider the case of hidden SU(Nc) gauge interactions that link the Planck mass to the condensation of a scalar bilinear operator that is nonminimally coupled to curvature. The effective theory at energies below the Planck mass contains two scalar fields: the pseudo-Nambu-Goldstone boson of spontaneously broken scale invariance (the dilaton) and a gravitational scalar degree of freedom that originates from the R2 term in the effective action (the scalaron). We compute the effective potential for the coupled dilaton-scalaron system at one-loop order and demonstrate that it can be used to successfully realize a stage of slow-roll inflation in the early Universe. Remarkably enough, our predictions for the primordial scalar and tensor power spectra interpolate between those of standard R2 inflation and linear chaotic inflation. For comparatively small gravitational couplings, we thus obtain a spectral index ns≃0.97 and a tensor-to-scalar ratio as large as r≃0.08. | ||
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