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Maldacena's consistency relation (eqs. 4.5–4.7): ⟨ζζζ⟩/(Pζ(k1)Pζ(k3))→−ns\langle\zeta\zeta\zeta\rangle/(P_\zeta(k_1)P_\zeta(k_3))\to-n_s⟨ζζζ⟩/(Pζ​(k1​)Pζ​(k3​))→−ns​ as k3→0k_3\to0k3​→0

Proved
Maldacena2003.squeezed_limit_consistency_relation

by Lucas · Oct 12, 2026 · Mathlib 0df444a (Lean v4.33.1)

cosmologyinflationmathematical-physics

Let ρ˙∗>0\dot\rho_*>0ρ˙​∗​>0, ϕ˙∗≠0\dot\phi_*\ne0ϕ˙​∗​=0, ϕ¨∗\ddot\phi_*ϕ¨​∗​ real, and k>0k>0k>0. Let Bζ(k1,k2,k3)B_\zeta(k_1,k_2,k_3)Bζ​(k1​,k2​,k3​) be the leading slow-roll three-scalar correlator of eqs. (4.5)–(4.6), PζP_\zetaPζ​ the scalar power spectrum (2.20), and nsn_sns​ the scalar tilt (2.22). Then, as (k2,k3)→(k,0)(k_2,k_3)\to(k,0)(k2​,k3​)→(k,0) through pairs for which (k,k2,k3)(k,k_2,k_3)(k,k2​,k3​) is a momentum triangle with positive sides,

Bζ(k,k2,k3)Pζ(k) Pζ(k3)  ⟶  − ns.\frac{B_\zeta(k,k_2,k_3)}{P_\zeta(k)\,P_\zeta(k_3)} \;\longrightarrow\; -\,n_s .Pζ​(k)Pζ​(k3​)Bζ​(k,k2​,k3​)​⟶−ns​.

In words: when one momentum is much smaller than the other two, the three-point function of ζ\zetaζ equals −ns-n_s−ns​ times the product of the two-point functions, ⟨ζk⃗1ζk⃗2ζk⃗3⟩∼−ns⟨ζk⃗3ζ−k⃗3⟩′⟨ζk⃗1ζk⃗2⟩′\langle\zeta_{\vec k_1}\zeta_{\vec k_2}\zeta_{\vec k_3}\rangle\sim-n_s\langle\zeta_{\vec k_3}\zeta_{-\vec k_3}\rangle'\langle\zeta_{\vec k_1}\zeta_{\vec k_2}\rangle'⟨ζk1​​ζk2​​ζk3​​⟩∼−ns​⟨ζk3​​ζ−k3​​⟩′⟨ζk1​​ζk2​​⟩′. This is the single-field consistency relation, eq. (4.7), recovered from the general formula (4.5)–(4.6).

Formalization Note Mpl=1M_{pl}=1Mpl​=1, H∗=ρ˙∗H_*=\dot\rho_*H∗​=ρ˙​∗​, the factor (2π)3δ3(∑k⃗i)(2\pi)^3\delta^3(\sum\vec k_i)(2π)3δ3(∑ki​) is dropped, and the horizon-crossing times ∗*∗, ∗′*'∗′ are identified at leading order in slow roll. The limit is taken in R2\mathbb R^2R2 within the momentum-triangle set; momentum conservation forces k2→kk_2\to kk2​→k.

Preamble
import Mathlib
import Definitions.Def_Maldacena2003_InflationDefs
open Filter Topology
Formal statement
namespace Maldacena2003

theorem squeezed_limit_consistency_relation (ρd φd φdd k : ℝ)
    (hρ : 0 < ρd) (hφ : φd ≠ 0) (hk : 0 < k) :
    Tendsto
      (fun p : ℝ × ℝ => zetaBispectrum ρd φd φdd k p.1 p.2
        / (zetaPowerSpectrum ρd φd k * zetaPowerSpectrum ρd φd p.2))
      (𝓝[{p : ℝ × ℝ | IsMomentumTriangle k p.1 p.2}] (k, 0))
      (𝓝 (-scalarTilt ρd φd φdd)) := by sorry

end Maldacena2003
Source
J. Maldacena, Non-Gaussian features of primordial fluctuations in single field inflationary models, JHEP 05 (2003) 013, https://doi.org/10.1088/1126-6708/2003/05/013 (arXiv:astro-ph/0210603), pp. 16–17, eqs. (4.5)–(4.7); also p. 7, eqs. (2.20), (2.22)
Human review
  • Endorsed by Shuze Chen · Oct 13, 2026

    Confirmed by the moderator at approval.

  • Endorsed by Lucas · Oct 13, 2026

    Confirmed by the mission captain (proposal self-audit).

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