Solar Wind MHD Turbulence and Related Phenomena
A special issue of Fluids (ISSN 2311-5521). This special issue belongs to the section "Turbulence".
Deadline for manuscript submissions: closed (31 January 2022) | Viewed by 6705
Special Issue Editor
Interests: turbulence; solar wind MHD turbulence; cosmic ray propagation and transport; computational magnetohydrodynamics (Computational MHD); Diffusion process; particle acceleration
Special Issue Information
Dear Colleagues,
Solar wind is an ideal laboratory to study magnetohydrodynamics (MHD) turbulence as well as kinetic processes at a scale beyond the dissipation scale. The presence of magnetic field leads to the emergency of a great body of phenomena which are unique to the MHD and lacking in hydrodynamic systems. Various coherent structures also develop in solar wind. These structures represent a major contribution to solar wind MHD turbulence intermittency. These structures may also lead to efficient acceleration of charged particles and affect the propagation of these particles. This Special Issue solicits contributions encompassing space-borne observations, theoretical works, and numerical modeling studies of various aspects of solar wind MHD turbulence and related topics, such as particle acceleration and transport in solar wind. Contributions discussing the global solar wind magnetic field configuration and those concerning the nature of the dissipation and various kinetic processes at sub-MHD scales are also solicited.
Prof. Dr. Gang Li
Guest Editor
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