Regulation of the solar wind electron heat flux from 1 to 5 AU: Ulysses observations

1994 ◽  
Vol 99 (A12) ◽  
pp. 23401 ◽  
Author(s):  
Earl E. Scime ◽  
Samuel J. Bame ◽  
William C. Feldman ◽  
S. Peter Gary ◽  
John L. Phillips ◽  
...  
Keyword(s):  
Heat Flux ◽  
Solar Wind ◽  
Electron Heat ◽  
Solar Wind Electron

Bidirectional solar wind electron heat flux and hemispherically symmetric polar rain

1986 ◽  
Vol 91 (A10) ◽  
pp. 11352 ◽  
Author(s):  
J. T. Gosling ◽  
D. N. Baker ◽  
S. J. Bame ◽  
R. D. Zwickl
Keyword(s):  
Heat Flux ◽  
Solar Wind ◽  
Electron Heat ◽  
Polar Rain ◽  
Solar Wind Electron

Latitudinal variations in the solar wind electron heat flux

1995 ◽  
Vol 72 (1-2) ◽  
pp. 105-108 ◽  
Author(s):  
Earl E. Scime ◽  
Samuel J. Bame ◽  
John L. Phillips ◽  
Andre Balogh
Keyword(s):  
Heat Flux ◽  
Solar Wind ◽  
Electron Heat ◽  
Latitudinal Variations ◽  
Solar Wind Electron

Parameters of solar wind electron heat-flux pitch-angle distributions and IMF topologies

2004 ◽  
Vol 31 (22) ◽  
Author(s):  
W. M. Feuerstein ◽  
D. E. Larson ◽  
J. G. Luhmann ◽  
R. P. Lin ◽  
S. W. Kahler ◽  
...  
Keyword(s):  
Heat Flux ◽  
Solar Wind ◽  
Pitch Angle ◽  
Electron Heat ◽  
Solar Wind Electron

Latitudinal Variations in the Solar Wind Electron Heat Flux

1995 ◽  
pp. 105-108
Author(s):  
Earl E. Scime ◽  
Samuel J. Bame ◽  
John L. Phillips ◽  
Andre Balogh
Keyword(s):  
Heat Flux ◽  
Solar Wind ◽  
Electron Heat ◽  
Latitudinal Variations ◽  
Solar Wind Electron

Bidirectional solar wind electron heat flux events

1987 ◽  
Vol 92 (A8) ◽  
pp. 8519 ◽  
Author(s):  
J. T. Gosling ◽  
D. N. Baker ◽  
S. J. Bame ◽  
W. C. Feldman ◽  
R. D. Zwickl ◽  
...  
Keyword(s):  
Heat Flux ◽  
Solar Wind ◽  
Electron Heat ◽  
Solar Wind Electron

scholarly journals The electron heat flux in the polar solar wind: Ulysses observations

1999 ◽  
Vol 26 (14) ◽  
pp. 2129-2132 ◽  
Author(s):  
Earl E. Scime ◽  
Allen E. Badeau ◽  
J. E. Littleton
Keyword(s):  
Heat Flux ◽  
Solar Wind ◽  
Electron Heat

Electron heat flux constraints in the solar wind

1999 ◽  
Vol 6 (6) ◽  
pp. 2607-2612 ◽  
Author(s):  
S. Peter Gary ◽  
Ruth M. Skoug ◽  
William Daughton
Keyword(s):  
Heat Flux ◽  
Solar Wind ◽  
Electron Heat

Skew-Kappa distribution functions & whistler-heat flux instability in the solar wind

2021 ◽  
Author(s):  
Bea Zenteno-Quinteros ◽  
Adolfo F. Viñas ◽  
Pablo S. Moya
Keyword(s):  
Heat Flux ◽  
Solar Wind ◽  
Electron Velocity ◽  
Marginal Stability ◽  
Threshold Condition ◽  
Kappa Distribution ◽  
Particle Interactions ◽  
Whistler Mode ◽  
Electron Heat ◽  
Wave Particle Interactions

<p>Electron velocity distributions in the solar wind are known to have field-aligned skewness, which has been observationally characterized by the presence of secondary populations such as the halo and strahl electron components. This non-thermal feature provides energy for the excitation of electromagnetic instabilities that may play a role in regulating the electron heat flux in the solar wind by wave-particle interactions. Among the wave modes excited in regulating the electron non-thermal features is the whistler-mode and its so-called whistler heat-flux instability (WHFI). In this work, we use kinetic linear theory to analyze the stability of the WHFI in a solar wind like plasma where the electrons are described as a single population modeled by a Kappa distribution to which an asymmetry term has been added. We solve the dispersion relation numerically for the parallel propagating whistler-mode and study its linear stability for different plasma parameters. We also show the marginal stability thresholds for this instability as a function of the electron beta and the parallel electron heat flux and present a threshold condition for instability that can be modeled to compare with observational data. The principal result is that the WHFI can develop in this system; however, the heat flux parameter is not a good predictor of how unstable this wave mode will be. This is because different plasma states, with different stability to WHFI, can have the same initial heat flux. Thus, systems with high <img title="This is the rendered form of the equation. You can not edit this directly. Right click will give you the option to save the image, and in most browsers you can drag the image onto your desktop or another program." src="https://latex.codecogs.com/gif.latex?q_%7B%5Cparallel%20e%7D/q_0"> can be stable enough to WHFI so that it cannot effectively modify the heat flux values through wave-particle interactions</p>

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