Non-minimal M-flation
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Springer
Received: January 30, Revised: June 8, Accepted: June 20, Published: July 31,
2020 2020 2020 2020
Amjad Ashoorioona and Kazem Rezazadeha,b a
School of Physics, Institute for Research in Fundamental Sciences (IPM), P.O. Box 19395-5531, Tehran, Iran b Department of Physics, University of Kurdistan, Pasdaran Street, P.O. Box 66177-15175, Sanandaj, Iran
E-mail: [email protected], [email protected] Abstract: We show how in a matrix inflationary model in which there is a non-minimal coupling between the matrix inflatons and gravity — hence dubbed Non-M-flation — some of the disadvantages of the minimal model can be avoided. In particular, the number of D3 branes can be reduced substantially to . O(100), which can alleviate the “potential” backreaction problem of large number of D3 branes on the background geometry. This is achieved by values of non-minimal coupling of order few hundred, which is much smaller than that of Higgs Inflation. The prediction of the model in the symmetry breaking part of the potential, which is a local attractor and can support eternal inflation, is compatible with the latest PLANCK results. In contrast to the minimal model, the spectator fields can partially or completely reheat the universe, depending on the symmetry-breaking vacuum expectation value and the non-minimal coupling parameter. We also comment on how the presence of gauge species keep the UV cutoff at around the Planck scale in the Einstein frame and, in contrast to the Higgs inflation, the problem of field displacements beyond the cutoff does not occur. Keywords: Cosmology of Theories beyond the SM, D-branes, M(atrix) Theories ArXiv ePrint: 1909.09806
c The Authors. Open Access, Article funded by SCOAP3 .
https://doi.org/10.1007/JHEP07(2020)244
JHEP07(2020)244
Non-minimal M-flation
Contents 1 Introduction
1
2 M -flation: a review 2.1 Background dynamics 2.2 Spectrum of spectators
4 4 6
3 Shortcomings of M -flation
7 10 10 11 15 17
5 Isocurvature spectra in non-M M -flation 5.1 Scalar isocurvature perturbations 5.2 Gauge isocurvature perturbations
18 18 20
6 Preheating in non-M M -flation 6.1 Scalar preheat fields 6.2 Gauge preheat fields
21 22 30
7 UV cutoff in non-M M -flation
35
8 Conclusions
38
A Non-M M -flation in the limit ξ 1
40
B Revising the Higgs inflation predictions
42
1
Introduction
Embedding the paradigm of inflation in the landscape of string theory, soon turned out to be a tedious task, despite how rich and vast the landscape looked like in the inception of its formulation. From two classes of small and large single field models, only the former [1] was thought to be possible to formulate in the string theory until about a decade ago [2], before the devise of monodromy inflation [3, 4]. In such single moduli models, the stabilization of volume modulus generically, couples the inflaton conformally to gravity, causing the notorious η-problem. This happens despite — and in fact because of — the large warping of the internal manifold, produced by internal fluxes. Before monodro
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