Fig. 3: Perpendicular wavenumber dependence of the compensated spectra, parallel wavenumber and nonlinearity parameter.
From: Identification of the weak-to-strong transition in Alfvénic turbulence from space plasma
a, \({k}_{\perp }^{\;5/3}{E}_{\mathrm{B}_\mathrm{A}}({k}_{\perp })\) versus k⊥. The dashed line represents the scaling \({k}_{\perp }^{\;5/3}{E}_{\mathrm{B}_\mathrm{A}}({k}_{\perp })\propto {k}_{\perp }^{\;5/3-2}\). To facilitate comparison with proton velocity fluctuations, magnetic field fluctuations are in Alfvén speed units. b, Variation of k∥ versus k⊥. The dashed line represents the scaling \({k}_{\parallel }\propto {k}_{\perp }^{\;2/3}\). The horizontal dotted line marks k∥ = 7 × 10−5 km−1. c, \({\chi }_{\mathrm{B}_\mathrm{A}}({k}_{\perp },{k}_{\parallel })\) spectrum calculated using the dataset for η < 30°. There are four zones: (1) 5 × 10−5 < k⊥ < 1.6 × 10−4 km−1, (2) 1.6 × 10−4 < k⊥ < 3 × 10−4 km−1, (3) 3 × 10−4 < k⊥ < 7 × 10−4 km−1 and (4) 7 × 10−4 < k⊥ < 1 × 10−3 km−1. The first, second and third vertical dotted lines are around the maximum of \({k}_{\perp }^{\;5/3}{E}_{\mathrm{B}_\mathrm{A}}({k}_{\perp })\), the beginning and the end of flattened \({k}_{\perp }^{\;5/3}{E}_{\mathrm{B}_\mathrm{A}}({k}_{\perp })\), respectively.
