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Are Moduli Vacuum Expectation Values or Parameters?

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arxiv 2502.07883 v1 pith:ELXJ7NOG submitted 2025-02-11 hep-th gr-qc

classification hep-thgr-qc
keywords modulivaluesdifferenttheoryasymptoticpointcorrespondexpectation
verification ladder T0 review T1 audit T2 compute T3 formal
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Banks has argued that the moduli of string theory are not vacuum expectation values but parameters. We offer a different perspective on this question. Given two different points P and Q in the moduli space, we shall regard them as different vacua of the same underlying theory if in a theory where the asymptotic values of the moduli correspond to the point P, we can perform an experiment that can determine the spectrum and S-matrix of a theory where the asymptotic values of the moduli correspond to the point Q. We argue that in asymptotically flat space-time, this can be achieved by taking a charged black hole in the limit of large mass and charges. In this limit the local geometry at any point outside the horizon is indistinguishable from flat space-time. However the moduli vary slowly over the entire region so that their values at faraway points can differ by order unity. Therefore, by sending out experimental teams to different regions outside the horizon, an asymptotic observer can measure the spectrum and S-matrix for different values of the moduli.

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Cited by 4 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Tame Complexity of Effective Field Theories in the Quantum Gravity Landscape

    hep-th 2026-01 conditional novelty 7.0 of 10

    Effective field theories consistent with quantum gravity are conjectured to have uniformly bounded 'tame complexity', a quantitative measure of the information needed to specify them.

  2. The Fate of Black Hole-Induced Moduli Excursions in the Presence of Scalar Potentials

    hep-th 2026-07 conditional novelty 6.0 of 10

    Black-hole moduli throats survive or fail according to how a potential’s force, sign, oscillations, or barrier distance behave along the GHS scalar trajectory, not by the mere presence of a mass.

  3. A Menagerie of Wormholes and Cosmologies in the Gravitational Path Integral

    hep-th 2026-02 unverdicted novelty 6.0 of 10

    The paper identifies a variety of Euclidean saddle solutions including wormholes and oscillatory configurations in Einstein-Scalar-Maxwell models, demonstrates how oscillations are controlled by lifting flat potential...

  4. Perturbative K\"ahler Moduli Inflation

    hep-th 2025-06 reject novelty 6.0 of 10

    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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