2020/12/09 by George Livadiotis, Maher A. Dayeh, Gary P. Zank · 1 citation
Physics and Astronomy · #physics.space-ph
paper · pdf · doi:10.3847/1538-4357/abc5c3
16 pages, 12 figures
arxiv created 2020/12/09 · arxiv updated 2021/01/06
The paper presents a new method for deriving turbulent heating of the solar wind using plasma moments and magnetic field data. We develop the method and then apply it to compute the turbulent heating of the solar wind proton plasma at 1AU. The method employs two physical properties of the expanding solar wind plasma, the wave-particle thermodynamic equilibrium, and the transport of entropic rate. We analyze plasma moments and field datasets taken from Wind S/C, in order to compute (i) the fluctuating magnetic energy, (ii) the corresponding correlation length, and (iii) the turbulent heating rate. We identify their relationships with the solar wind speed, as well as the variation of these relationships relative to solar wind and interplanetary coronal mass ejection plasma.