When electric-type flux threads compact extra dimensions, a quantum nucleation event can break a flux line and initiate a cascade that unwinds many units of flux. Here, we present a novel mechanism for inflation based on this phenomenon. From the 4D point of view, the cascade begins with the formation of a bubble containing an open Friedmann-Robertson-Walker cosmology, but the vacuum energy inside the bubble is initially only slightly reduced, and subsequently decreases gradually throughout the cascade. If the initial flux number Q0≳O(100), during the cascade the universe can undergo N≳. 60 efolds of inflationary expansion with gradually decreasing Hubble constant, producing a nearly scale-invariant spectrum of adiabatic density perturbations with amplitude and tilt consistent with observation, and a potentially observable level of non-Gaussianity and tensor modes. The power spectrum has a small oscillatory component that does not decay away during inflation, with a period set approximately by the light-crossing time of the compact dimension(s). Since the ingredients are fluxes threading compact dimensions, this mechanism fits naturally into the string landscape, but does not appear to suffer from the eta problem or require fine-tuning (beyond the usual anthropic requirement of small vacuum energy after reheating). © 2013 .

Inflation from flux cascades / D'Amico, Guido; Gobbetti, Roberto; Kleban, Matthew; Schillo, Marjorie L.. - In: PHYSICS LETTERS. SECTION B. - ISSN 0370-2693. - 725:4-5(2013), pp. 218-222. [10.1016/j.physletb.2013.07.050]

Inflation from flux cascades

D'Amico, Guido;
2013

Abstract

When electric-type flux threads compact extra dimensions, a quantum nucleation event can break a flux line and initiate a cascade that unwinds many units of flux. Here, we present a novel mechanism for inflation based on this phenomenon. From the 4D point of view, the cascade begins with the formation of a bubble containing an open Friedmann-Robertson-Walker cosmology, but the vacuum energy inside the bubble is initially only slightly reduced, and subsequently decreases gradually throughout the cascade. If the initial flux number Q0≳O(100), during the cascade the universe can undergo N≳. 60 efolds of inflationary expansion with gradually decreasing Hubble constant, producing a nearly scale-invariant spectrum of adiabatic density perturbations with amplitude and tilt consistent with observation, and a potentially observable level of non-Gaussianity and tensor modes. The power spectrum has a small oscillatory component that does not decay away during inflation, with a period set approximately by the light-crossing time of the compact dimension(s). Since the ingredients are fluxes threading compact dimensions, this mechanism fits naturally into the string landscape, but does not appear to suffer from the eta problem or require fine-tuning (beyond the usual anthropic requirement of small vacuum energy after reheating). © 2013 .
Inflation from flux cascades / D'Amico, Guido; Gobbetti, Roberto; Kleban, Matthew; Schillo, Marjorie L.. - In: PHYSICS LETTERS. SECTION B. - ISSN 0370-2693. - 725:4-5(2013), pp. 218-222. [10.1016/j.physletb.2013.07.050]
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/11381/2856395
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