Fig. 2: Comparison between wavenumber distributions of Alfvénic magnetic energy \({\hat{\boldsymbol{D}}}_{{\mathbf{B}}_{\mathbf{A}}}{\boldsymbol{(}}{\boldsymbol{k}}_{\perp},{\boldsymbol{k}}_{\boldsymbol{\parallel}}{\boldsymbol{)}}\) and the theoretical energy spectra \({\hat{\boldsymbol{I}}}_{\mathbf{A}}{\boldsymbol{(}}{\boldsymbol{k}}_{\perp},{\boldsymbol{k}}_{\parallel}{\boldsymbol{)}}\).
From: Identification of the weak-to-strong transition in Alfvénic turbulence from space plasma
a, 2D spectral image of \({\hat{D}}_{\mathrm{B}_\mathrm{A}}({k}_{\perp },{k}_{\parallel })\) with a high resolution (400 × 400 bins). b, 2D filled contours of \({\hat{D}}_{\mathrm{B}_\mathrm{A}}({k}_{\perp },{k}_{\parallel })\) with low-resolution binning (150 × 150 bins), to clarify the contours. In each panel, \({\hat{I}}_\mathrm{A}({k}_{\perp },{k}_{\parallel })\) at L0 ≈ 4.6 × 104 km is displayed by colour contours with black dashed curves with the same colour map as \({\hat{D}}_{\mathrm{B}_\mathrm{A}}({k}_{\perp },{k}_{\parallel })\). The black dotted curves mark \(k=\sqrt{{k}_{\parallel }^{2}+{k}_{\perp }^{2}}=0.01/{d}_{i}\) and 0.03/di. These figures utilize the dataset for η < 30°.
