Speaker
Description
The phenomenon of energy dissipation in collisionless plasmas such as the solar wind remains a subject of incomplete understanding within the scientific community. Central to this enigma is the intermittent nature of magnetic structures, which seems to play a pivotal role in the energy cascade process. Achieving a comprehensive comprehension of energy transfer and dissipation in the solar wind necessitates a precise characterization of its intermittency. The advent of forthcoming multi-spacecraft missions holds promise for shedding new light on this intricate phenomenon. However, harnessing the potential of multi-point data necessitates the development of innovative data analysis methodologies, alongside rigorous cross-validation efforts. In this investigation, we concentrate on the latter aspect, delving into the intricacies of intermittency through a 3D simulation of anisotropic plasma turbulence via two distinct methodologies. Specifically, we employ both the conventional single-spacecraft partial variance increments technique and a novel multi-point partial variance increments technique. Through comparative analysis, we scrutinize the efficacy of these approaches and investigate their sensitivity to variations in the angle between the spacecraft configuration's travel direction and the background magnetic field $\mathbf{B_0}$.
