Collisionless Damping at Electron Scales in Solar Wind Turbulence
Abstract
The dissipation of turbulence in the weakly collisional solar wind plasma is governed by unknown kinetic mechanisms. Two candidates have been suggested to play an important role in the dissipation, collisionless damping via wave-particle interactions and dissipation in small-scale current sheets. High resolution spacecraft measurements of the turbulent magnetic energy spectrum provide important constraints on the dissipation mechanism. The limitations of popular fluid and hybrid numerical schemes for simulation of the dissipation of solar wind turbulence are discussed, and instead a three-dimensional kinetic approach is recommended. We present a three-dimensional nonlinear gyrokinetic simulation of solar wind turbulence at electron scales that quantitatively reproduces the exponential form of the turbulent magnetic energy spectrum measured in the solar wind. A weakened cascade model that accounts for nonlocal interactions and collisionless Landau damping also quantitatively agrees with the observed exponential form. Finally, these results establish that a turbulent cascade of kinetic Alfvén waves that is terminated by collisionless Landau damping is sufficient to explain the observed magnetic energy spectrum in the dissipation range of solar wind turbulence.
- Authors:
-
- Univ. of Iowa, Iowa City, IA (United States). Dept. of Physics and Astronomy
- Univ. of Maryland, College Park, MD (United States). Dept. of Physics
- Publication Date:
- Research Org.:
- Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States). Oak Ridge Leadership Computing Facility (OLCF)
- Sponsoring Org.:
- USDOE Office of Science (SC)
- OSTI Identifier:
- 1565020
- Grant/Contract Number:
- AC05-00OR22725
- Resource Type:
- Accepted Manuscript
- Journal Name:
- The Astrophysical Journal
- Additional Journal Information:
- Journal Volume: 774; Journal Issue: 2; Journal ID: ISSN 0004-637X
- Publisher:
- Institute of Physics (IOP)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; astronomy & astrophysics; plasmas; solar wind; turbulence
Citation Formats
TenBarge, J. M., Howes, G. G., and Dorland, W. Collisionless Damping at Electron Scales in Solar Wind Turbulence. United States: N. p., 2013.
Web. doi:10.1088/0004-637x/774/2/139.
TenBarge, J. M., Howes, G. G., & Dorland, W. Collisionless Damping at Electron Scales in Solar Wind Turbulence. United States. https://doi.org/10.1088/0004-637x/774/2/139
TenBarge, J. M., Howes, G. G., and Dorland, W. Mon .
"Collisionless Damping at Electron Scales in Solar Wind Turbulence". United States. https://doi.org/10.1088/0004-637x/774/2/139. https://www.osti.gov/servlets/purl/1565020.
@article{osti_1565020,
title = {Collisionless Damping at Electron Scales in Solar Wind Turbulence},
author = {TenBarge, J. M. and Howes, G. G. and Dorland, W.},
abstractNote = {The dissipation of turbulence in the weakly collisional solar wind plasma is governed by unknown kinetic mechanisms. Two candidates have been suggested to play an important role in the dissipation, collisionless damping via wave-particle interactions and dissipation in small-scale current sheets. High resolution spacecraft measurements of the turbulent magnetic energy spectrum provide important constraints on the dissipation mechanism. The limitations of popular fluid and hybrid numerical schemes for simulation of the dissipation of solar wind turbulence are discussed, and instead a three-dimensional kinetic approach is recommended. We present a three-dimensional nonlinear gyrokinetic simulation of solar wind turbulence at electron scales that quantitatively reproduces the exponential form of the turbulent magnetic energy spectrum measured in the solar wind. A weakened cascade model that accounts for nonlocal interactions and collisionless Landau damping also quantitatively agrees with the observed exponential form. Finally, these results establish that a turbulent cascade of kinetic Alfvén waves that is terminated by collisionless Landau damping is sufficient to explain the observed magnetic energy spectrum in the dissipation range of solar wind turbulence.},
doi = {10.1088/0004-637x/774/2/139},
journal = {The Astrophysical Journal},
number = 2,
volume = 774,
place = {United States},
year = {Mon Aug 26 00:00:00 EDT 2013},
month = {Mon Aug 26 00:00:00 EDT 2013}
}
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