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Moduli Stabilization and Inflation in Type IIB/F-theory

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arxiv 1901.05075 v1 pith:3ZN7J57C submitted 2019-01-15 hep-th gr-qchep-ph

classification hep-thgr-qchep-ph
keywords inflationmoduliahlerf-theorypartsittertypebranes
verification ladder T0 review T1 audit T2 compute T3 formal
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abstract

In the first part of this talk, a short overview of the ongoing debate on the existence of de Sitter vacua in string theory is presented. In the second part, the moduli stabilisation and inflation are discussed in the context of type IIB/F-theory. Considering a configuration of three intersecting $D7$ branes with fluxes, it is shown that higher loop effects inducing logarithmic corrections to the K\"ahler potential can stabilise the K\"ahler moduli in a de Sitter Vacuum. When a new Fayet-Iliopoulos term is included, it is also possible to generate the required number of e-foldings and satisfy the conditions for slow-roll inflation.

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Cited by 4 Pith papers

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  1. Tetra-quadric CY Threefold and Assisted Fibre Inflation

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    Three Kähler moduli on a tetra-quadric CY orientifold collectively drive assisted fibre inflation with individual shifts near 2.2 M_p instead of the effective 5.7 M_p.

  2. On Calabi-Yau Threefolds For Unified LVS Inflation

    hep-th 2026-06 unverdicted novelty 6.0 of 10

    A database scan identifies 2+14+45 Calabi-Yau threefolds with specified fibration and divisor structures that unify three LVS Kähler moduli inflation models.

  3. Fire at the Tip of the Throat: Hagedorn Phase after brane-antibrane inflation?

    hep-th 2026-06 unverdicted novelty 5.0 of 10

    In perturbatively moduli-stabilized brane-antibrane inflation, a modest fraction of annihilation energy into visible open strings can trigger a Hagedorn phase that suppresses ΔN_eff when the SM throat string scale is ...

  4. Assisted Fibre Inflation in Perturbative LVS

    hep-th 2025-06 unverdicted novelty 4.0 of 10

    Multi-field fibre inflation in perturbative LVS uses collective dynamics of several moduli to achieve viable cosmology with sub-Planckian individual field ranges given by total range divided by sqrt(n).

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