Convective instability in a solar flux tube. I - Nonlinear calculations for an adiabatic inviscid fluid

1984 ◽  
Vol 285 ◽  
pp. 851 ◽  
Author(s):  
S. Sirajul Hasan
Keyword(s):  
Flux Tube ◽  
Convective Instability ◽  
Solar Flux ◽  
Inviscid Fluid

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

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

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

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

A Numerical Model of MHD Waves in a 3D Twisted Solar Flux Tube

Solar Physics ◽  
2015 ◽  
Vol 290 (7) ◽  
pp. 1909-1922 ◽  
Author(s):  
K. Murawski ◽  
A. Solov’ev ◽  
J. Kraśkiewicz
Keyword(s):  
Numerical Model ◽  
Flux Tube ◽  
Solar Flux ◽  
Mhd Waves

Activated Prominences; Mechanisms for Activation and Eruption

1979 ◽  
Vol 44 ◽  
pp. 307-313
Author(s):  
D.S. Spicer
Keyword(s):  
Pressure Gradient ◽  
Density Gradient ◽  
Current Density ◽  
Convective Instability ◽  
Tearing Mode ◽  
Magnetic Shear ◽  
Long Wavelength ◽  
Ideal Mhd ◽  
Gradient Change ◽  
Accelerated Particles

A possible relationship between the hot prominence transition sheath, increased internal turbulent and/or helical motion prior to prominence eruption and the prominence eruption (“disparition brusque”) is discussed. The associated darkening of the filament or brightening of the prominence is interpreted as a change in the prominence’s internal pressure gradient which, if of the correct sign, can lead to short wavelength turbulent convection within the prominence. Associated with such a pressure gradient change may be the alteration of the current density gradient within the prominence. Such a change in the current density gradient may also be due to the relative motion of the neighbouring plages thereby increasing the magnetic shear within the prominence, i.e., steepening the current density gradient. Depending on the magnitude of the current density gradient, i.e., magnetic shear, disruption of the prominence can occur by either a long wavelength ideal MHD helical (“kink”) convective instability and/or a long wavelength resistive helical (“kink”) convective instability (tearing mode). The long wavelength ideal MHD helical instability will lead to helical rotation and thus unwinding due to diamagnetic effects and plasma ejections due to convection. The long wavelength resistive helical instability will lead to both unwinding and plasma ejections, but also to accelerated plasma flow, long wavelength magnetic field filamentation, accelerated particles and long wavelength heating internal to the prominence.

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