Extends the σ-flip framework to stellar evolution, revealing implications for dark matter interactions.
We extend the σ-flip framework of Paper 1 [1] to the full lifecycle of stellar evolution. The sameU(1)_σ gauge symmetry that produces dark matter via freeze-in at T_QCD governs a subdominant bidirectional exchange between dark and visible sectors throughout stellar evolution:a reverse σ-flip (σ: −1 → +1) in dense molecular cloud cores contributes to stellar nucleation,while the direct σ-flip (σ: +1 → −1) at stellar death acts as an astrophysical probe of the freezein mechanism. This paper introduces two free parameters — the reverse σ-flip efficiency ε_revand the reverse threshold density ρ_c^reverse — and shows that both are independentlyconstrained by the observed star formation rate and the Jeans instability criterion, respectively.The direct σ-flip efficiency ε_direct ≡ ε = 10 ⁶ is not a new parameter: it is inherited from the ⁻kinetic mixing of Paper 1. From these inputs we derive the Initial Mass Function slope α = 2.32± 0.15, consistent with the Salpeter value of 2.35 [9]; a reinterpretation of the Chandrasekharlimit as the σ-flip activation threshold; and the Baryonic Tully-Fisher slope 3.7 ± 0.4. Wedemonstrate explicitly that the stellar-cycle contributions to Ω_DM are sub-dominant by sevento eleven orders of magnitude, preserving the freeze-in result of Paper 1. Six new quantitativepredictions are derived for JWST, DUNE, Euclid, Rubin LSST, Gaia, and SKA.
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Leandro de Oliveira (2026) studied this question.
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