scholarly journals Electron beam formation by small-scale oblique inertial Alfvén waves

1999 ◽  
Vol 104 (A8) ◽  
pp. 17233-17249 ◽  
Author(s):  
A. E. Clark ◽  
C. E. Seyler
Keyword(s):  
Electron Beam ◽  
Alfven Waves ◽  
Alfvén Waves ◽  
Small Scale ◽  
Beam Formation ◽  
Inertial Alfvén Waves

Solar coronal heating by Alfvén waves in bi-kappa distributed plasma

2019 ◽  
Vol 491 (2) ◽  
pp. 2403-2412 ◽  
Author(s):  
Imran A Khan ◽  
Z Iqbal ◽  
G Murtaza
Keyword(s):  
Distribution Function ◽  
Velocity Distribution ◽  
Particle Interaction ◽  
Velocity Distribution Function ◽  
Alfven Waves ◽  
Coronal Heating ◽  
Alfvén Waves ◽  
Heating Process ◽  
Thermal Features ◽  
Inertial Alfvén Waves

ABSTRACT In solar physics, there is a decades-old conundrum that is still unsolved. Why is the temperature of the corona so much larger than that of the surface of the Sun? To solve this, various approaches have been adopted so far, but they have certain limitations. In the present analysis, we invoke the standard Vlasov model and the steady-state Poynting theorem to unlock the mysterious coronal heating mechanism in terms of inertial and kinetic Alfvén waves whose electromagnetic energies turn into heat during wave–particle interaction. The coronal plasmas that support these waves are modelled by a non-thermal bi-kappa velocity distribution function. The non-thermal distribution function, which is assumed to pre-exist in the system, strongly influences the wave-heating process. Particularly, during heating by the waves in the inertial limit, the non-thermal features of the distribution function give rise to a unique competition (which is entirely absent in the usual Maxwellian plasmas) between waves of different perpendicular wavenumbers (kx). For small kx, when either the non-thermal parameter κ or the electron parallel temperature T||e increases, the inertial Alfvén waves can efficiently heat the plasma in their immediate vicinity. However, for relatively large kx, an increase in either κ or T||e enables the inertial Alfvén waves to effectively heat the plasma in remote regions in the corona. Although such competition is not seen in the kinetic limit, the non-thermal features still seem to control the heating process. The possible explanations behind the above-mentioned cases are provided by the bi-kappa velocity distribution function, which holds vital clues as to how the non-thermal features, together with kx, dictate the resonance conditions that play a crucial role in the heating process.

SMALL-SCALE SOLAR WIND TURBULENCE DUE TO NONLINEAR ALFVÉN WAVES

2015 ◽  
Vol 812 (1) ◽  
pp. 69 ◽  
Author(s):  
Sanjay Kumar ◽  
R. P. Sharma ◽  
Y.-J. Moon
Keyword(s):  
Solar Wind ◽  
Alfven Waves ◽  
Alfvén Waves ◽  
Small Scale ◽  
Solar Wind Turbulence ◽  
Wind Turbulence

On the propagation of transversally small-scale standing Alfven waves in a three-dimensionally inhomogeneous magnetosphere

1995 ◽  
Vol 100 (A6) ◽  
pp. 9527 ◽  
Author(s):  
Dmitrii Yu. Klimushkin ◽  
Anatolii S. Leonovich ◽  
Vitalii A. Mazur
Keyword(s):  
Alfven Waves ◽  
Alfvén Waves ◽  
Small Scale

On the dispersion and damping of kinetic and inertial Alfvén waves in Cairns distributed plasmas

2019 ◽  
Vol 26 (6) ◽  
pp. 062101
Author(s):  
S. Ayaz ◽  
Imran A. Khan ◽  
G. Murtaza
Keyword(s):  
Alfven Waves ◽  
Alfvén Waves ◽  
Inertial Alfvén Waves

scholarly journals Nonlinear interactions between three inertial Alfvén waves

2007 ◽  
Vol 73 (1) ◽  
pp. 9-13 ◽  
Author(s):  
G. BRODIN ◽  
L. STENFLO ◽  
P. K. SHUKLA
Keyword(s):  
Temperature Effects ◽  
Alfven Waves ◽  
Alfvén Waves ◽  
Nonlinear Interactions ◽  
Resonant Coupling ◽  
Inertial Alfvén Waves

Abstract.The resonant coupling between Alfvén waves is reconsidered. New results are found for cold magnetoplasmas where temperature effects are negligible.

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