Electron energy transport in the solar wind: Ulysses observations

1996 ◽  
Author(s):  
Earl E. Scime ◽  
S. Peter Gary ◽  
John L. Phillips ◽  
Andre Balogh ◽  
Denise Lengyel-Frey
Keyword(s):  
Solar Wind ◽  
Electron Energy ◽  
Energy Transport

Erratum: Revisiting Nonlocal Electron-Energy Transport in Inertial-Fusion Conditions [Phys. Rev. Lett.98, 095002 (2007)]

2007 ◽  
Vol 98 (14) ◽  
Author(s):  
G. Schurtz ◽  
S. Gary ◽  
S. Hulin ◽  
C. Chenais-Popovics ◽  
J.-C. Gauthier ◽  
...  
Keyword(s):  
Electron Energy ◽  
Energy Transport ◽  
Inertial Fusion

scholarly journals High-latitude electromagnetic and particle energy flux during an event with sustained strongly northward IMF

2005 ◽  
Vol 23 (4) ◽  
pp. 1295-1310 ◽  
Author(s):  
H. Korth ◽  
B. J. Anderson ◽  
H. U. Frey ◽  
C. L. Waters
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Energy Flux ◽  
High Latitude ◽  
Energy Transport ◽  
Small Region ◽  
Radial Component ◽  
Particle Energy ◽  
Electromagnetic Energy ◽  
Viscous Interaction

Abstract. We present a case study of a prolonged interval of strongly northward orientation of the interplanetary magnetic field on 16 July 2000, 16:00-19:00 UT to characterize the energy exchange between the magnetosphere and ionosphere for conditions associated with minimum solar wind-magnetosphere coupling. With reconnection occurring tailward of the cusp under northward IMF conditions, the reconnection dynamo should be separated from the viscous dynamo, presumably driven by the Kelvin-Helmholtz (KH) instability. Thus, these conditions are also ideal for evaluating the contribution of a viscous interaction to the coupling process. We derive the two-dimensional distribution of the Poynting vector radial component in the northern sunlit polar ionosphere from magnetic field observations by the constellation of Iridium satellites together with drift meter and magnetometer observations from the Defense Meteorological Satellite Program (DMSP) F13 and F15 satellites. The electromagnetic energy flux is then compared with the particle energy flux obtained from auroral images taken by the far-ultraviolet (FUV) instrument on the Imager for Magnetopause to Aurora Global Exploration (IMAGE) spacecraft. The electromagnetic energy input to the ionosphere of 51 GW calculated from the Iridium/DMSP observations is eight times larger than the 6 GW due to particle precipitation all poleward of 78° MLAT. This result indicates that the energy transport is significant, particularly as it is concentrated in a small region near the magnetic pole, even under conditions traditionally considered to be quiet and is dominated by the electromagnetic flux. We estimate the contributions of the high and mid-latitude dynamos to both the Birkeland currents and electric potentials finding that high-latitude reconnection accounts for 0.8 MA and 45kV while we attribute <0.2MA and ~5kV to an interaction at lower latitudes having the sense of a viscous interaction. Given that these conditions are ideal for the occurrence of the KH instability at the magnetopause and hence the viscous interaction, this result suggests that the viscous interaction is a small contributor to coupling solar wind energy to the magnetosphere-ionosphere system.

scholarly journals Dispersion relation analysis of turbulent magnetic field fluctuations in fast solar wind

2013 ◽  
Vol 31 (11) ◽  
pp. 1949-1955 ◽  
Author(s):  
C. Perschke ◽  
Y. Narita ◽  
S. P. Gary ◽  
U. Motschmann ◽  
K.-H. Glassmeier
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
High Speed ◽  
Energy Transport ◽  
Normal Modes ◽  
Frequency Dispersion ◽  
Dispersion Relations ◽  
Wave Number ◽  
Magnetic Fluctuations ◽  
Speed Solar Wind

Abstract. Physical processes of the energy transport in solar wind turbulence are a subject of intense studies, and different ideas exist to explain them. This manuscript describes the investigation of dispersion properties in short-wavelength magnetic turbulence during a rare high-speed solar wind event with a flow velocity of about 700 km s−1 using magnetic field and ion data from the Cluster spacecraft. Using the multi-point resonator technique, the dispersion relations (i.e., frequency versus wave-number values in the solar wind frame) of turbulent magnetic fluctuations with wave numbers near the inverse ion inertial length are determined. Three major results are shown: (1) the wave vectors are uniformly quasi-perpendicular to the mean magnetic field; (2) the fluctuations show a broad range of frequencies at wavelengths around the ion inertial length; and (3) the direction of propagation at the observed wavelengths is predominantly in the sunward direction. These results suggest the existence of high-frequency dispersion relations partly associated with normal modes on small scales. Therefore nonlinear energy cascade processes seem to be acting that are not described by wave–wave interactions.

scholarly journals The Kelvin-Helmholtz Instability From the Perspective of Hybrid Simulations

2021 ◽  
Vol 8 ◽  
Author(s):  
P. A. Delamere ◽  
N. P. Barnes ◽  
X. Ma ◽  
J. R. Johnson
Keyword(s):  
Solar Wind ◽  
Surface Waves ◽  
Energy Transport ◽  
Helmholtz Instability ◽  
Flow Shear ◽  
Planetary Magnetospheres ◽  
Dayside Magnetopause ◽  
Hybrid Simulations

The flow shear-driven Kelvin-Helmholtz (KH) instability is ubiquitous in planetary magnetospheres. At Earth these surface waves are important along the dawn and dusk flanks of the magnetopause boundary while at Jupiter and Saturn the entire dayside magnetopause boundary can exhibit KH activity due to corotational flows in the magnetosphere. Kelvin-Helmholtz waves can be a major ingredient in the so-called viscous-like interaction with the solar wind. In this paper, we review the KH instability from the perspective of hybrid (kinetic ions, fluid electrons) simulations. Many of the simulations are based on parameters typically found at Saturn’s magnetopause boundary, but the results can be generally applied to any KH-unstable situation. The focus of the discussion is on the ion kinetic scale and implications for mass, momentum, and energy transport at the magnetopause boundary.

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