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− e− 1 ν2 (κ2 2+κ2 3) i · (κ1κ2)−1 Z d3⃗ξ (1 + ξ2)−4ϕ⃗ κ1(⃗ξ)ϕ⃗ κ2(⃗ξ)ϕ∗ ⃗ κ3(⃗ξ) 2 ≡ λ2ρ2 g 16π2m5ak2g α(ν, ˜N) , (47) where α(ν, ˜N) is a dimensionless numerical factor, κ3 is

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hep-ph 1

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2025 1

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Axion Star Bosenova in Axion Miniclusters

hep-ph · 2025-08-20 · unverdicted · novelty 5.0

Axion stars in miniclusters can reach bosenova conditions within the age of the Universe for QCD axions when initial overdensity exceeds roughly 100, once self-interaction effects are included.

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  • Axion Star Bosenova in Axion Miniclusters hep-ph · 2025-08-20 · unverdicted · none · ref 1

    Axion stars in miniclusters can reach bosenova conditions within the age of the Universe for QCD axions when initial overdensity exceeds roughly 100, once self-interaction effects are included.