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Swampland Distance Conjecture, Inflation and $\alpha$-attractors
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abstract
The Swampland Distance Conjecture (SDC) constraints the dynamics emerging at infinite distances in field space of any effective field theory consistent with quantum gravity. It provides a relation between the cut-off in energies and the field range which, as we show, in the context of inflation it yields a universal upper bound on the inflaton excursion in terms of the tensor-to-scalar ratio, measured at typical CMB scales. In this note, we investigate the interplay between the SDC and the emergent inflationary physics around infinite distances singularities in string theory, with a special look at its significance for the $\alpha$-attractor scenario of inflation. We show that the conjecture itself suggests that inflation may arise as an infinite distance phenomenon with the asymptotic kinetic structure typical of $\alpha$-attractors. Furthermore, we argue that a proper string realisation of these cosmological models in Calabi-Yau manifolds should occur around infinite field distance singularities. However, such constructions typically imply that inflation should not take place in the limit where the inflaton kinetic term develops a pole but rather in the opposite regime. Finally, we study the constraints that the SDC poses on $\alpha$-attractors and show that they still leave considerable room for compatibility with observations.
Forward citations
Cited by 13 Pith papers
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The Boundary of Symmetric Moduli Spaces and the Swampland Distance Conjecture
For locally symmetric moduli spaces satisfying a compactifiability constraint, every infinite-distance limit produces an exponentially light tower of states, with decay rates forming the convex hull of the weights of ...
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Ultraviolet completion of Starobinsky inflation
A supergravity construction using two chiral superfields embeds arbitrary F(R) gravity as a UV completion of Starobinsky inflation, stabilized by the dilaton and consistent with swampland constraints in a heterotic st...
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Inflationary Particle Production and the Swampland
Tower-induced corrections to inflationary observables scale as (H/Λsp)^{2+p} and are negligible whenever H≪Λsp.
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Global Asymptotics, the Swampland Conjectures, and Preheating of String Moduli
Global asymptotic shape, not just local curvature, controls tachyonic self-resonant preheating of string moduli, and stochastic light-tower effects mostly smear existing resonance bands.
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Corrections to inflationary models induced by non-minimal coupling between scalar field and curvature
A power-law non-minimal scalar-curvature coupling F=(H/λ)^{2n} is shown to deform inflationary potentials and to rescale the tensor-to-scalar ratio r→(1−n)r_E while preserving the n_T=−r/8 consistency relation.
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Corrections to inflationary models induced by non-minimal coupling between scalar field and curvature
Power-law non-minimal coupling F=(H/λ)^{2n} deforms inflationary potentials, shifts r and n_S while preserving n_T=-r/8 and GR-like reheating, enabling r(1-n_S) classification of models against Planck/ACT data.
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Quintessential $\alpha$-attractors fit DESI
α-attractor quintessence models approximate axion-like potentials and fit DESI dynamical dark energy data, preferring α of order 1 via a simple fa-α relation.
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Long Inflation Screens Euclidean-Wormhole Initial States
Long inflation screens Euclidean wormhole initial states from the CMB, turning them into Bunch-Davies predictions and providing a bound on inflationary duration via visibility limits on Bogoliubov excitations.
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Pure Natural Inflation Passes the ACT
Pure natural inflation remains viable against latest ACT+DESI constraints, with a non-trivial fraction of parameter space allowed under standard reheating scenarios.
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Assisted Fibre Inflation in Perturbative LVS
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Pure Natural Inflation Passes the ACT
Pure natural inflation remains compatible with ACT+DESI constraints on ns and r for small positive and mildly negative p under instantaneous and perturbative reheating.
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The Wave Function of the Universe and Inflation
Rearranging the Wheeler-DeWitt equation defines the inflaton potential in terms of an arbitrary wave-function phase and amplitude; nothing constrains that wave function, so the potential is relabeled rather than deriv...
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