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Kahler Moduli Inflation

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arxiv hep-th/0509012 v2 pith:R2CQU3LO submitted 2005-09-01 hep-th astro-phhep-ph

Joseph P. Conlon , Fernando Quevedo This is my paper
classification hep-thastro-phhep-ph
keywords inflationkahlercalabi-yaucompactificationsconditionsinflationaryitselfleast
verification ladder T0 review T1 audit T2 compute T3 formal
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We show that under general conditions there is at least one natural inflationary direction for the Kahler moduli of type IIB flux compactifications. This requires a Calabi-Yau which has h^{2,1}>h^{1,1}>2 and for which the structure of the scalar potential is as in the recently found exponentially large volume compactifications. We also need - although these conditions may be relaxed - at least one Kahler modulus whose only non-vanishing triple-intersection is with itself and which appears by itself in the non-perturbative superpotential. Slow-roll inflation then occurs without a fine tuning of parameters, evading the eta problem of F-term inflation. In order to obtain COBE-normalised density perturbations, the stabilised volume of the Calabi-Yau must be O(10^5-10^7) in string units, and the inflationary scale M_{infl} ~ 10^{13} GeV. We find a robust model independent prediction for the spectral index of 1 - 2/N_e = 0.960 - 0.967, depending on the number of efoldings.

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Cited by 6 Pith papers

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  4. Perturbative K\"ahler Moduli Inflation

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    Two classes of slow-roll inflation potentials, V0(1+C1 φ^(2/3)) and V0(1-C2 φ^(-2/3)), are derived from perturbative Kähler moduli stabilization and give r below 10^-2 and 10^-8.

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