Dust heating by Alfvén waves using non-Maxwellian distribution function

2015 ◽  
Vol 22 (8) ◽  
pp. 082902 ◽  
Author(s):  
K. Zubia ◽  
H. A. Shah ◽  
P. H. Yoon
Keyword(s):  
Distribution Function ◽  
Alfven Waves ◽  
Maxwellian Distribution ◽  
Alfvén Waves ◽  
Maxwellian Distribution Function

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.

The Drifted Maxwellian Distribution Function in InSb

1967 ◽  
Vol 20 (2) ◽  
pp. K135-K139 ◽  
Author(s):  
G. Jones ◽  
G. Smith ◽  
A. R. Beattle
Keyword(s):  
Distribution Function ◽  
Maxwellian Distribution ◽  
Maxwellian Distribution Function

The Excitation Equilibrium in the Solar Corona and Non-Maxwellian Electron Distributions

1994 ◽  
Vol 144 ◽  
pp. 435-438
Author(s):  
E. Dzifčáková
Keyword(s):  
Distribution Function ◽  
Solar Corona ◽  
Maxwellian Distribution ◽  
Collisional Excitation ◽  
Excitation Coefficient ◽  
Electron Distributions ◽  
Maxwellian Distribution Function ◽  
Excitation Equilibrium

AbstractWe demonstrate the influence of an electron non-Maxwellian distribution function on the collisional excitation coefficient and, as an example, on the excitation equilibrium of Fe XIV in the solar corona. The results can be used for specific applications in the solar corona, especially in the active corona, where deviations from Maxwellian distribution can be significant.

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