Publisher’s Note: Nature of Subproton Scale Turbulence in the Solar Wind [Phys. Rev. Lett.110, 225002 (2013)]

2013 ◽  
Vol 110 (25) ◽  
Author(s):  
C. H. K. Chen ◽  
S. Boldyrev ◽  
Q. Xia ◽  
J. C. Perez
Keyword(s):  
Solar Wind ◽  
Scale Turbulence

scholarly journals Nature of Subproton Scale Turbulence in the Solar Wind

2013 ◽  
Vol 110 (22) ◽  
Author(s):  
C. H. K. Chen ◽  
S. Boldyrev ◽  
Q. Xia ◽  
J. C. Perez
Keyword(s):  
Solar Wind ◽  
Scale Turbulence

A Turbulent Heliosheath Driven by Rayleigh Taylor Instability

2021 ◽  
Author(s):  
Merav Opher ◽  
James Drake ◽  
Gary Zank ◽  
Gabor Toth ◽  
Erick Powell ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Large Scale ◽  
Neutral Atom ◽  
Solar Magnetic Field ◽  
Characteristic Time Scale ◽  
Rayleigh Taylor Instability ◽  
Scale Turbulence ◽  
Magnetohydrodynamic Simulations ◽  
Rt Instability

Abstract The heliosphere is the bubble formed by the solar wind as it interacts with the interstellar medium (ISM). Studies show that the solar magnetic field funnels the heliosheath solar wind (the shocked solar wind at the edge of the heliosphere) into two jet-like structures1-2. Magnetohydrodynamic simulations show that these heliospheric jets become unstable as they move down the heliotail1,3 and drive large-scale turbulence. However, the mechanism that produces of this turbulence had not been identified. Here we show that the driver of the turbulence is the Rayleigh-Taylor (RT) instability caused by the interaction of neutral H atoms streaming from the ISM with the ionized matter in the heliosheath (HS). The drag between the neutral and ionized matter acts as an effective gravity which causes a RT instability to develop along the axis of the HS magnetic field. A density gradient exists perpendicular to this axis due to the confinement of the solar wind by the solar magnetic field. The characteristic time scale of the instability depends on the neutral H density in the ISM and for typical values the growth rate is ~ 3 years. The instability destroys the coherence of the heliospheric jets and magnetic reconnection ensues, allowing ISM material to penetrate the heliospheric tail. Signatures of this instability should be observable in Energetic Neutral Atom (ENA) maps from future missions such as IMAP4. The turbulence driven by the instability is macroscopic and potentially has important implications for particle acceleration.

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.

Weakened Magnetization and Onset of Large-scale Turbulence in the Young Solar Wind—Comparisons of Remote Sensing Observations with Simulation

2018 ◽  
Vol 856 (2) ◽  
pp. L39 ◽  
Author(s):  
Rohit Chhiber ◽  
Arcadi V. Usmanov ◽  
Craig E. DeForest ◽  
William H. Matthaeus ◽  
Tulasi N. Parashar ◽  
...  
Keyword(s):  
Remote Sensing ◽  
Solar Wind ◽  
Large Scale ◽  
Scale Turbulence

scholarly journals Radio Source Scintillations Through Comet Tails Revisited: Comet Wilson (1987)

1990 ◽  
Vol 43 (6) ◽  
pp. 801 ◽  
Author(s):  
OB Slee ◽  
AD Bobra ◽  
D Waldron ◽  
J Lim
Keyword(s):  
Solar Wind ◽  
Transition Region ◽  
Large Scale ◽  
Fold Increase ◽  
Density Variation ◽  
Scintillation Index ◽  
Small Scale ◽  
Negative Results ◽  
Electron Density Variation ◽  
Scale Turbulence

Observations of the quasars 0606-795 and 0637-752 as the tail of Comet Wilson swept across them on May 1 and May 2, 1987, showed a three-fold increase in scintillation index over that of nearby compact radio sources outside the tail. Two scintillation regimes have been identified: (1) small-scale turbulence of 10-40 km develops near the tail-axis; (2) large-scale turbulence of 90-350 km is present in the off-axis transition region between the tail plasma and solar wind. At a distance 0�12 AU downstream from the nucleus the r.m.s. electron-density variation in these turbules is 4-8 cm-3 on axis and 0�8-1� 7 cm-3 in the transition region between the tail and the solar wind. The reported negative results from earlier comets are shown to be of doubtful significance.

scholarly journals Observational Evidence for Solar Wind Proton Heating by Ion‐Scale Turbulence

2020 ◽  
Vol 47 (18) ◽  
Author(s):  
G. Q. Zhao ◽  
Y. Lin ◽  
X. Y. Wang ◽  
D. J. Wu ◽  
H. Q. Feng ◽  
...  
Keyword(s):  
Solar Wind ◽  
Observational Evidence ◽  
Solar Wind Proton ◽  
Scale Turbulence

scholarly journals Dissipation-scale turbulence in the solar wind

2007 ◽  
Author(s):  
G. G. Howes ◽  
S. C. Cowley ◽  
W. Dorland ◽  
G. W. Hammett ◽  
E. Quataert ◽  
...  
Keyword(s):  
Solar Wind ◽  
Dissipation Scale ◽  
Scale Turbulence

scholarly journals Modeling of short scale turbulence in the solar wind

2005 ◽  
Vol 12 (1) ◽  
pp. 75-81 ◽  
Author(s):  
V. Krishan ◽  
S. M. Mahajan
Keyword(s):  
Solar Wind ◽  
High Frequency ◽  
Low Frequency ◽  
Magnetic Fluctuation ◽  
Quadratic Invariants ◽  
Frame Work ◽  
Scale Turbulence ◽  
Shear Alfven Waves ◽  
Equipartition Of Energy ◽  
Hall Mhd

Abstract. The solar wind serves as a laboratory for investigating magnetohydrodynamic turbulence under conditions irreproducible on the terra firma. Here we show that the frame work of Hall magnetohydrodynamics (HMHD), which can support three quadratic invariants and allows nonlinear states to depart fundamentally from the Alfvénic, is capable of reproducing in the inertial range the three branches of the observed solar wind magnetic fluctuation spectrum - the Kolmogorov branch f -5/3 steepening to f -α1 with on the high frequency side and flattening to f -1 on the low frequency side. These fluctuations are found to be associated with the nonlinear Hall-MHD Shear Alfvén waves. The spectrum of the concomitant whistler type fluctuations is very different from the observed one. Perhaps the relatively stronger damping of the whistler fluctuations may cause their unobservability. The issue of equipartition of energy through the so called Alfvén ratio acquires a new status through its dependence, now, on the spatial scale.

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