Pith. sign in

Thus, for a = [0, 1], the T α-attractor models vary by α = [1, 1 2 ]

As compared to T α-attractor models with the potential VE ∼ tanh2n(ψ/ √ 6α) [6], we can identify the model parameters by 1 +a = 1 α, n = 2 · 2024

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The pole inflation from broken non-compact isometry in Weyl gravity

hep-ph · 2024-11-25 · conditional · novelty 5.0

Weyl gravity with a broken SO(1,N) scalar isometry produces pole inflation whose predictions vary with a parameter a, which also fixes the Weyl gauge boson mass and allows a ~10 MeV Weyl photon dark matter candidate.

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  • The pole inflation from broken non-compact isometry in Weyl gravity hep-ph · 2024-11-25 · conditional · none · ref 6

    Weyl gravity with a broken SO(1,N) scalar isometry produces pole inflation whose predictions vary with a parameter a, which also fixes the Weyl gauge boson mass and allows a ~10 MeV Weyl photon dark matter candidate.