Effects of Solar Activity on Taylor Scale and Correlation Scale in Solar Wind Magnetic Fluctuations

• Published in: Astrophysical journal. Letters 2020-08, Vol.899 (2), p.L32
• Main Authors: Zhou, G., He, H.-Q., Wan, W.
• Format: Article
• Language: English
• Subjects: Advanced Composition Explorer; Cluster spacecraft; Correlation coefficient; Correlation coefficients; Fluctuations; Fluid dynamics; Fluid flow; Interplanetary magnetic field; Interplanetary magnetic field fluctuations; Interplanetary medium; Interplanetary turbulence; Magnetic fields; Magnetic variations; Plasma turbulence; Solar activity; Solar cycle; Solar magnetic fields; Solar wind; Solar wind turbulence; Space plasmas; Spacecraft; Sunspot numbers; Sunspots; Time correlation functions
• ISSN: 2041-8205; 2041-8213
• DOI: 10.3847/2041-8213/abaaa9

The correlation scale and the Taylor scale are evaluated for interplanetary magnetic field fluctuations from two-point, single time correlation function using the Advanced Composition Explorer (ACE), Wind, and Cluster spacecraft data during the time period from 2001 to 2017, which covers over an entire solar cycle. The correlation scale and the Taylor scale are respectively compared with the sunspot number to investigate the effects of solar activity on the structure of the plasma turbulence. Our studies show that the Taylor scale increases with the increasing sunspot number, which indicates that the Taylor scale is positively correlated with the energy cascade rate, and the correlation coefficient between the sunspot number and the Taylor scale is 0.92. However, these results are not consistent with the traditional knowledge in hydrodynamic dissipation theories. One possible explanation is that in the solar wind, the fluid approximation fails at the spatial scales near the dissipation ranges. Therefore, the traditional hydrodynamic turbulence theory is incomplete for describing the physical nature of the solar wind turbulence, especially at the spatial scales near the kinetic dissipation scales.