Autocorrelation and Cross-Correlation of MHD Turbulence across IP Shock: Multispacecraft Analysis

Turbulent processes play a key role in the dynamics of solar wind plasma fluctuations, governing energy transfer within the heliosphere and driving particle acceleration. In this study, we aim to investigate the nature of large- and small-scale fluctuations in the upstream and downstream regions of interplanetary shocks. By analyzing magnetic field fluctuations using both traditional and recently developed methods, we examine changes in correlation length, Taylor scale, and Reynolds number from upstream to downstream regions. Plasma and magnetic field measurements from the ACE, WIND, and DSCOVR missions are utilized in this analysis. Correlation lengths are determined using autocorrelation and cross-correlation functions applied across data from the three spacecraft. When analyzing the Reynolds number, we observe a decrease in values when transitioning from upstream to downstream regions, suggesting turbulence resetting in the case under consideration. Building on the findings of a case study, we extend our investigation by performing a statistical analysis of these parameters across multiple shocks.