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Solar Wind MHD Turbulence and Related Phenomena

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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 5836

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Special Issue Editor

Prof. Dr. Gang Li

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Guest Editor

Space Science Department, The University of Alabama in Huntsville, 301 Sparkman Drive, Cramer Research Hall, Room 2037, Huntsville, AL 35899, USA
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

Manuscript Submission Information

Manuscripts should be submitted online at www.mdpi.com by registering and logging in to this website. Once you are registered, click here to go to the submission form. Manuscripts can be submitted until the deadline. All submissions that pass pre-check are peer-reviewed. Accepted papers will be published continuously in the journal (as soon as accepted) and will be listed together on the special issue website. Research articles, review articles as well as short communications are invited. For planned papers, a title and short abstract (about 100 words) can be sent to the Editorial Office for announcement on this website.

Submitted manuscripts should not have been published previously, nor be under consideration for publication elsewhere (except conference proceedings papers). All manuscripts are thoroughly refereed through a single-blind peer-review process. A guide for authors and other relevant information for submission of manuscripts is available on the Instructions for Authors page. Fluids is an international peer-reviewed open access monthly journal published by MDPI.

Please visit the Instructions for Authors page before submitting a manuscript. The Article Processing Charge (APC) for publication in this open access journal is 1800 CHF (Swiss Francs). Submitted papers should be well formatted and use good English. Authors may use MDPI's English editing service prior to publication or during author revisions.

Published Papers (2 papers)

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Research

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13 pages, 391 KiB

Open AccessArticle

Statistical Error for Cosmic Rays Modulation Evaluated by SDE Backward in Time Method for 1D Model

by Viacheslav Mykhailenko and Pavol Bobik

Fluids 2022, 7(2), 46; https://doi.org/10.3390/fluids7020046 - 19 Jan 2022

Cited by 4 | Viewed by 1910

Abstract

The propagation of cosmic rays through the heliosphere has been solved for more than half a century by stochastic methods based on Ito’s lemma. This work presents the estimation of statistical error of solution of Fokker–Planck equation by the 1D backward in time stochastic differential equations method. The error dependence on simulation statistics and energy is presented for different combinations of input parameters. The 1% precision criterion in mean value units of intensity standard deviation is defined as a function of solar wind velocity and diffusion coefficient value. Full article

(This article belongs to the Special Issue Solar Wind MHD Turbulence and Related Phenomena)

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Review

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32 pages, 1753 KiB

Open AccessReview

The Transport and Evolution of MHD Turbulence throughout the Heliosphere: Models and Observations

by Laxman Adhikari, Gary P. Zank and Lingling Zhao

Fluids 2021, 6(10), 368; https://doi.org/10.3390/fluids6100368 - 19 Oct 2021

Cited by 23 | Viewed by 3066

Abstract

A detailed study of solar wind turbulence throughout the heliosphere in both the upwind and downwind directions is presented. We use an incompressible magnetohydrodynamic (MHD) turbulence model that includes the effects of electrons, the separation of turbulence energy into proton and electron heating, the electron heat flux, and Coulomb collisions between protons and electrons. We derive expressions for the turbulence cascade rate corresponding to the energy in forward and backward propagating modes, the fluctuating kinetic and magnetic energy, the normalized cross-helicity, and the normalized residual energy, and calculate the turbulence cascade rate from 0.17 to 75 au in the upwind and downwind directions. Finally, we use the turbulence transport models to derive cosmic ray (CR) parallel and perpendicular mean free paths (mfps) in the upwind and downwind heliocentric directions. We find that turbulence in the upwind and downwind directions is different, in part because of the asymmetric distribution of new born pickup ions in the two directions, which results in the CR mfps being different in the two directions. This is important for models that describe the modulation of cosmic rays by the solar wind. Full article

(This article belongs to the Special Issue Solar Wind MHD Turbulence and Related Phenomena)

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