Scale-Dependent Turbulent Dynamics and Phase-Space Behavior of the Stable Atmospheric Boundary Layer

Abstract

The structure of turbulent dynamics in a stable atmospheric boundary layer was studied by means of a phase-space description. Data from the CASES-99 experiment, decomposed in local modes (with increasing time scale) using empirical mode decomposition, were analyzed in order to extract the proper time lag and the embedding dimension of the phase-space manifold, and subsequently to estimate their scale-dependent correlation dimension. Results show that the dynamics are low-dimensional and anisotropic for a large scale, where the flow is dominated by the bulk motion. Then, they become progressively more high-dimensional while transiting into the inertial sub-range. Finally, they reach three-dimensionality in the range of scales compatible with the center of the inertial sub-range, where the phase-space-filling turbulent fluctuations dominate the dynamics.

Statistical study of electron density turbulence and ion-cyclotron waves in the inner heliosphere: Solar Orbiter observations

“…However, the general features of the various IMFs depend on the specific process under analysis. For a turbulent field (Huang et al 2008;Carbone et al 2016aCarbone et al , 2018Carbone et al , 2020a or for a multifractal process (Carbone et al 2010;Sorriso-Valvo et al 2017), the characteristic mean period grows exponentially as τ j = αγ j , where • represents an ensemble average (in this case, average over time).…”

Statistical study of electron density turbulence and ion-cyclotron waves in the inner heliosphere: Solar Orbiter observations

“…However, the general features of the various IMFs depend on the specific process under analysis. For a turbulent field (Huang et al 2008;Carbone et al 2016aCarbone et al , 2018Carbone et al , 2020a or for a multifractal process (Carbone et al 2010;Sorriso-Valvo et al 2017), the characteristic mean period grows exponentially as τ j = αγ j , where • represents an ensemble average (in this case, average over time). The basis γ can be evaluated empirically from the IMFs.…”

Statistical Analysis of Field-Aligned Alfvénic Turbulence and Intermittency in Fast Solar Wind

“…When the EMD is applied on turbulent processes [36][37][38] or multifractal processes [39,40], it intrinsically acts as a dyadic filter bank [41][42][43][44], where each IMF captures a narrow band in frequency space, and their characteristic period τ j follows an exponential law of the form: τ j = α × γ j , where γ = 2 for an exact dyadic decomposition. The dashed line in the central panel of Figure 2 represents the least square fit of the exponential relation obtained for τ j , with γ = 1.97 ± 0.01, showing very good agreement with the theoretical expectation.…”