Structures and Intermittency in Small Scales Solar Wind Turbulence

2010 ◽  
Author(s):  
Fouad Sahraoui ◽  
Melvyn Goldstein ◽  
M. Maksimovic ◽  
K. Issautier ◽  
N. Meyer-Vernet ◽  
...  
Keyword(s):  
Solar Wind ◽  
Solar Wind Turbulence ◽  
Small Scales ◽  
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.

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

Solar wind turbulence: Connections with energetic particles

New Astronomy ◽  
2021 ◽  
Vol 83 ◽  
pp. 101507
Author(s):  
Sean Oughton ◽  
N. Eugene Engelbrecht
Keyword(s):  
Solar Wind ◽  
Energetic Particles ◽  
Solar Wind Turbulence ◽  
Wind Turbulence

scholarly journals Solar cycle changes in the geo-effectiveness of small-scale solar wind turbulence measured by Wind and ACE at 1 AU

2007 ◽  
Vol 25 (5) ◽  
pp. 1183-1197 ◽  
Author(s):  
M. L. Parkinson ◽  
R. C. Healey ◽  
P. L. Dyson
Keyword(s):  
Solar Wind ◽  
Solar Cycle ◽  
Solar Minimum ◽  
Large Scale ◽  
Small Scale ◽  
Scaling Exponent ◽  
Mhd Turbulence ◽  
Scaling Exponents ◽  
Solar Wind Turbulence ◽  
Wind Turbulence

Abstract. Multi-scale structure of the solar wind in the ecliptic at 1 AU undergoes significant evolution with the phase of the solar cycle. Wind spacecraft measurements during 1995 to 1998 and ACE spacecraft measurements during 1997 to 2005 were used to characterise the evolution of small-scale (~1 min to 2 h) fluctuations in the solar wind speed vsw, magnetic energy density B2, and solar wind ε parameter, in the context of large-scale (~1 day to years) variations. The large-scale variation in ε most resembled large-scale variations in B2. The probability density of large fluctuations in ε and B2 both had strong minima during 1995, a familiar signature of solar minimum. Generalized Structure Function (GSF) analysis was used to estimate inertial range scaling exponents aGSF and their evolution throughout 1995 to 2005. For the entire data set, the weighted average scaling exponent for small-scale fluctuations in vsw was aGSF=0.284±0.001, a value characteristic of intermittent MHD turbulence (>1/4), whereas the scaling exponents for corresponding fluctuations in B2 and ε were aGSF=0.395±0.001 and 0.334±0.001, respectively. These values are between the range expected for Gaussian fluctuations (1/2) and Kolmogorov turbulence (1/3). However, the scaling exponent for ε changed from a Gaussian-Kolmogorov value of 0.373±0.005 during 1997 (end of solar minimum) to an MHD turbulence value of 0.247±0.004 during 2003 (recurrent fast streams). Changes in the characteristics of solar wind turbulence may be reproducible from one solar cycle to the next.

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