Spectral Exponents of Kinetic and Magnetic Energy Spectra in Solar Wind Turbulence

2007 ◽  
Vol 664 (1) ◽  
pp. 543-548 ◽  
Author(s):  
J. J. Podesta ◽  
D. A. Roberts ◽  
M. L. Goldstein
Keyword(s):  
Solar Wind ◽  
Magnetic Energy ◽  
Energy Spectra ◽  
Solar Wind Turbulence ◽  
Wind Turbulence

scholarly journals Kinetic scale turbulence and dissipation in the solar wind: key observational results and future outlook

2015 ◽  
Vol 373 (2041) ◽  
pp. 20140147 ◽  
Author(s):  
M. L. Goldstein ◽  
R. T. Wicks ◽  
S. Perri ◽  
F. Sahraoui
Keyword(s):  
Solar Wind ◽  
Magnetic Energy ◽  
Future Outlook ◽  
Turbulent Dissipation ◽  
Solar Wind Turbulence ◽  
Small Scales ◽  
Wind Turbulence ◽  
Scale Turbulence

Turbulence is ubiquitous in the solar wind. Turbulence causes kinetic and magnetic energy to cascade to small scales where they are eventually dissipated, adding heat to the plasma. The details of how this occurs are not well understood. This article reviews the evidence for turbulent dissipation and examines various diagnostics for identifying solar wind regions where dissipation is occurring. We also discuss how future missions will further enhance our understanding of the importance of turbulence to solar wind dynamics.

scholarly journals Two Correlations with Enhancement Near the Proton Gyroradius Scale in Solar Wind Turbulence: Parker Solar Probe (PSP) and Wind Observations

2022 ◽  
Vol 924 (2) ◽  
pp. 92
Author(s):  
G. Q. Zhao ◽  
Y. Lin ◽  
X. Y. Wang ◽  
H. Q. Feng ◽  
D. J. Wu ◽  
...  
Keyword(s):  
Solar Wind ◽  
Magnetic Energy ◽  
Data Sets ◽  
Absolute Value ◽  
Magnetic Energy Density ◽  
Solar Wind Turbulence ◽  
Proton Temperature ◽  
Wind Turbulence ◽  
First Time ◽  
Probe Mission

Abstract Based on the Parker Solar Probe mission, this paper presents the observations of two correlations in solar wind turbulence near the Sun for the first time, demonstrating the clear existence of the following two correlations. One is positive correlation between the proton temperature and turbulent magnetic energy density. The other is negative correlation between the spectral index and magnetic helicity. It is found that the former correlation has a maximum correlation coefficient (CC) at the wavenumber k ρ p ≃ 0.5 (ρ p being the proton thermal gyroradius), and the latter correlation has a maximum absolute value of CC at k ρ p ≃ 1.8. In addition, investigations based on 11 yr of Wind observations reveal that the dimensionless wavenumbers (k ρ p ) corresponding to the maximum (absolute) values of CC remain nearly the same for different data sets. These results tend to suggest that the two correlations enhanced near the proton gyroradius scale would be a common feature of solar wind turbulence.

Observational Test for a Random Sweeping Model in Solar Wind Turbulence

2016 ◽  
Vol 116 (12) ◽  
Author(s):  
C. Perschke ◽  
Y. Narita ◽  
U. Motschmann ◽  
K. H. Glassmeier
Keyword(s):  
Solar Wind ◽  
Observational Test ◽  
Solar Wind Turbulence ◽  
Wind Turbulence

Erratum: “3D Anisotropy of Solar Wind Turbulence, Tubes, or Ribbons?” (2018, ApJ, 853, 85)

2018 ◽  
Vol 867 (2) ◽  
pp. 168 ◽  
Author(s):  
Andrea Verdini ◽  
Roland Grappin ◽  
Olga Alexandrova ◽  
Sonny Lion
Keyword(s):  
Solar Wind ◽  
Solar Wind Turbulence ◽  
Wind Turbulence

scholarly journals Kinetic Cascade in Solar-wind Turbulence: 3D3V Hybrid-kinetic Simulations with Electron Inertia

2017 ◽  
Vol 846 (2) ◽  
pp. L18 ◽  
Author(s):  
Silvio Sergio Cerri ◽  
Sergio Servidio ◽  
Francesco Califano
Keyword(s):  
Solar Wind ◽  
Electron Inertia ◽  
Solar Wind Turbulence ◽  
Wind Turbulence

scholarly journals Solar Wind Turbulence from 1 to 45 au. IV. Turbulent Transport and Heating of the Solar Wind Using Voyager Observations

2020 ◽  
Vol 900 (2) ◽  
pp. 94 ◽  
Author(s):  
Zackary B. Pine ◽  
Charles W. Smith ◽  
Sophia J. Hollick ◽  
Matthew R. Argall ◽  
Bernard J. Vasquez ◽  
...  
Keyword(s):  
Solar Wind ◽  
Turbulent Transport ◽  
Solar Wind Turbulence ◽  
Wind Turbulence
Sign in / Sign up

Export Citation Format

Share Document