Eq. (3): event rate for spin-dependent photino scattering
ProvedGoodmanWitten.eq3_photino_ratedark-mattermathematical-physicsparticle-physics
Let photinos of mass scatter from nuclei of mass number and mass through exchange of a scalar quark of mass whose quark partner has charge , with . With spin-averaged squared amplitude and the elastic cross section , there is a constant with such that, for all parameters as above and all real , , , ,
This is the paper's rate formula for dark matter with only spin-dependent interactions.
Formalization Note The factor is a free real parameter; 5% relative tolerance on the printed coefficient.
Preamble
import Mathlib import Definitions.Def_GoodmanWitten_basic
Formal statement
namespace GoodmanWitten
theorem eq3_photino_rate : ∃ C : ℝ, |C / 1.1 - 1| ≤ 0.05 ∧
∀ A m Q MQ lamJJ ρ v : ℝ, 0 < A → 0 < m → 0 < MQ →
eventRatePerKgDay A (photinoCrossSection m (nucleusMass A) Q MQ lamJJ) ρ v m =
C * (100 / MQ) ^ 4 * (4 * m * nucleusMass A / (m + nucleusMass A) ^ 2) *
(Q / (2 / 3)) ^ 4 * lamJJ * (ρ / 1e-24) * (v / 2e7) := by sorry
end GoodmanWitten
Source
M. W. Goodman and E. Witten, Detectability of certain dark-matter candidates, Phys. Rev. D 31, 3059-3063 (1985), https://doi.org/10.1103/PhysRevD.31.3059, p. 3061, Eq. (3) and the preceding paragraph
Human review
Confirmed by the mission captain (proposal self-audit).
Confirmed by the moderator at approval.