Fig. 4: The k⊥ versus frest distributions of Alfvénic magnetic energy in the plasma flow frame.
From: Identification of the weak-to-strong transition in Alfvénic turbulence from space plasma
\({\hat{D}}_{\mathrm{B}_\mathrm{A}}({k}_{\perp},{f}_\mathrm{rest})={D}_{\mathrm{B}_\mathrm{A}}({k}_{\perp},{f}_\mathrm{rest})/{D}_{\mathrm{B}_\mathrm{A},\max}\) is normalized by the maximum magnetic energy in all (k⊥, frest) bins. The horizontal dotted lines represent theoretical Alfvén frequencies fA = ∣k∥VA∣/(2π), where k∥ ≈ 7 × 10−5 km−1 in zone 1 of Fig. 3b, and k∥ ≈ 1 × 10−4 km−1 in zone 1 of Supplementary Fig. 7b. The fA uncertainties are estimated by the standard deviation of VA (106 ± 11 km−1), illustrated by error bars on corresponding horizontal dotted lines. This figure utilizes the dataset for η < 30°.
