scholarly journals Numerical simulations of magnetic Kelvin–Helmholtz instability at a twisted solar flux tube

2016 ◽  
Vol 459 (3) ◽  
pp. 2566-2572 ◽  
Author(s):  
K. Murawski ◽  
P. Chmielewski ◽  
T.V. Zaqarashvili ◽  
E. Khomenko
Keyword(s):  
Numerical Simulations ◽  
Flux Tube ◽  
Solar Flux ◽  
Helmholtz Instability

Numerical simulations of three-dimensional magnetic swirls in a solar flux-tube

2014 ◽  
Vol 14 (7) ◽  
pp. 855-863 ◽  
Author(s):  
Piotr Chmielewski ◽  
Krzysztof Murawski ◽  
Alexandr A. Solov'ev
Keyword(s):  
Numerical Simulations ◽  
Flux Tube ◽  
Three Dimensional ◽  
Solar Flux

scholarly journals Numerical simulations of the lower solar atmosphere heating by two-fluid nonlinear Alfvén waves

2020 ◽  
Vol 639 ◽  
pp. A45
Author(s):  
B. Kuźma ◽  
D. Wójcik ◽  
K. Murawski ◽  
D. Yuan ◽  
S. Poedts
Keyword(s):  
Magnetic Flux ◽  
Numerical Simulations ◽  
Solar Atmosphere ◽  
Flux Tube ◽  
Alfven Waves ◽  
Alfven Wave ◽  
Magnetic Flux Tube ◽  
Alfvén Waves ◽  
Two Fluid ◽  
Lower Solar Atmosphere

Context. We present new insight into the long-standing problem of plasma heating in the lower solar atmosphere in terms of collisional dissipation caused by two-fluid Alfvén waves. Aims. Using numerical simulations, we study Alfvén wave propagation and dissipation in a magnetic flux tube and their heating effect. Methods. We set up 2.5-dimensional numerical simulations with a semi-empirical model of a stratified solar atmosphere and a force-free magnetic field mimicking a magnetic flux tube. We consider a partially ionized plasma consisting of ion + electron and neutral fluids, which are coupled by ion-neutral collisions. Results. We find that Alfvén waves, which are directly generated by a monochromatic driver at the bottom of the photosphere, experience strong damping. Low-amplitude waves do not thermalize sufficient wave energy to heat the solar atmospheric plasma. However, Alfvén waves with amplitudes greater than 0.1 km s−1 drive through ponderomotive force magneto-acoustic waves in higher atmospheric layers. These waves are damped by ion-neutral collisions, and the thermal energy released in this process leads to heating of the upper photosphere and the chromosphere. Conclusions. We infer that, as a result of ion-neutral collisions, the energy carried initially by Alfvén waves is thermalized in the upper photosphere and the chromosphere, and the corresponding heating rate is large enough to compensate radiative and thermal-conduction energy losses therein.

Particle propagation effects on wave growth in a solar flux tube

1986 ◽  
Vol 308 ◽  
pp. 424 ◽  
Author(s):  
S. M. White ◽  
D. B. Melrose ◽  
G. A. Dulk
Keyword(s):  
Flux Tube ◽  
Solar Flux ◽  
Wave Growth ◽  
Propagation Effects ◽  
Particle Propagation

A Quasi-One-Dimensional Model for a Solar Flux Tube

2002 ◽  
Vol 19 (8) ◽  
pp. 1217-1220
Author(s):  
Yang Zhi-Liang ◽  
Zhang Hong-Qi ◽  
Zhang Mei ◽  
Feng Xue-Shang
Keyword(s):  
Flux Tube ◽  
Solar Flux ◽  
Dimensional Model ◽  
One Dimensional

NUMERICAL SIMULATIONS OF PLASMA DYNAMICS IN THE VICINITY OF A RETRACTING FLUX TUBE

2016 ◽  
Vol 831 (1) ◽  
pp. 94 ◽  
Author(s):  
Roger B. Scott ◽  
Dana W. Longcope ◽  
David E. McKenzie
Keyword(s):  
Numerical Simulations ◽  
Flux Tube ◽  
Plasma Dynamics
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