Propagating MHD Waves in Coronal Plasma Waveguides

2012 ◽  
pp. 67-92
Keyword(s):  
Coronal Plasma ◽  
Mhd Waves ◽  
Plasma Waveguides

Numerical simulations of fast MHD waves in a coronal plasma

Solar Physics ◽  
1993 ◽  
Vol 144 (2) ◽  
pp. 255-266 ◽  
Author(s):  
K. Murawski ◽  
B. Roberts
Keyword(s):  
Numerical Simulations ◽  
Coronal Plasma ◽  
Mhd Waves

Numerical simulations of fast MHD waves in a coronal plasma

Solar Physics ◽  
1993 ◽  
Vol 143 (1) ◽  
pp. 89-105 ◽  
Author(s):  
K. Murawski ◽  
B. Roberts
Keyword(s):  
Numerical Simulations ◽  
Coronal Plasma ◽  
Mhd Waves

Numerical simulations of fast MHD waves in a coronal plasma

Solar Physics ◽  
1993 ◽  
Vol 145 (1) ◽  
pp. 65-75 ◽  
Author(s):  
K. Murawski ◽  
B. Roberts
Keyword(s):  
Numerical Simulations ◽  
Coronal Plasma ◽  
Mhd Waves

Viscous Damping of Non-Adiabatic MHD Waves in an Unbounded Solar Coronal Plasma

Solar Physics ◽  
2006 ◽  
Vol 236 (1) ◽  
pp. 137-153 ◽  
Author(s):  
Nagendra Kumar ◽  
Pradeep Kumar
Keyword(s):  
Coronal Plasma ◽  
Mhd Waves ◽  
Viscous Damping ◽  
Solar Coronal

Magnetohydrodynamic Waves in the Solar Corona

2020 ◽  
Vol 58 (1) ◽  
pp. 441-481 ◽  
Author(s):  
Valery M. Nakariakov ◽  
Dmitrii Y. Kolotkov
Keyword(s):  
Transport Coefficients ◽  
Theoretical Models ◽  
Oscillation Period ◽  
Magnetized Plasma ◽  
Coronal Plasma ◽  
Theoretical Research ◽  
Mhd Waves ◽  
Polytropic Index ◽  
Fast Wave ◽  
Plasma Parameters

The corona of the Sun is a unique environment in which magnetohydrodynamic (MHD) waves, one of the fundamental processes of plasma astrophysics, are open to a direct study. There is striking progress in both observational and theoretical research of MHD wave processes in the corona, with the main recent achievements summarized as follows: ▪  Both periods and wavelengths of the principal MHD modes of coronal plasma structures, such as kink, slow and sausage modes, are confidently resolved. ▪  Scalings of various parameters of detected waves and waveguiding plasma structures allow for the validation of theoretical models. In particular, kink oscillation period scales linearly with the length of the oscillating coronal loop, clearly indicating that they are eigenmodes of the loop. Damping of decaying kink and standing slow oscillations depends on the oscillation amplitudes, demonstrating the importance of nonlinear damping. ▪  The dominant excitation mechanism for decaying kink oscillations is associated with magnetized plasma eruptions. Propagating slow waves are caused by the leakage of chromospheric oscillations. Fast wave trains could be formed by waveguide dispersion. ▪  The knowledge gained in the study of coronal MHD waves provides ground for seismological probing of coronal plasma parameters, such as the Alfvén speed, the magnetic field and its topology, stratification, temperature, fine structuring, polytropic index, and transport coefficients.

Propagation and damping of slow MHD waves in a flowing viscous coronal plasma

2016 ◽  
Vol 361 (4) ◽  
Author(s):  
Nagendra Kumar ◽  
Anil Kumar ◽  
K. Murawski
Keyword(s):  
Coronal Plasma ◽  
Mhd Waves

Numerical simulations of fast MHD waves in a coronal plasma

Solar Physics ◽  
1993 ◽  
Vol 144 (1) ◽  
pp. 101-112 ◽  
Author(s):  
K. Murawski ◽  
B. Roberts
Keyword(s):  
Numerical Simulations ◽  
Coronal Plasma ◽  
Mhd Waves

scholarly journals Numerical Simulation of Twisted Solar Corona

1998 ◽  
Vol 185 ◽  
pp. 467-468
Author(s):  
S. Parhi ◽  
B.P. Pandey ◽  
M. Goossens ◽  
G.S. Lakhina
Keyword(s):  
Numerical Simulation ◽  
Wave Propagation ◽  
Solar Corona ◽  
Temperature Profile ◽  
Resonant Absorption ◽  
Wave Generation ◽  
Coronal Plasma ◽  
Mhd Waves ◽  
Coronal Temperature ◽  
Physical Picture

The solar corona supports a variety of waves generated by convective upwelling motion in the photosphere. In order to explain the observed coronal temperature profile, resonant absorption of MHD waves by coronal plasma (Goossens et al, 1995) has been proposed as a possible candidate. The physical picture is that the footpoint motion in the photosphere constantly stirs the coronal plasma leading to the MHD wave generation which is then resonantly absorbed producing the enhanced heating of the corona. Here we consider the problem of MHD wave propagation in a twisted solar corona.

Linear Visco-Resistive Computations of Magnetohydrodynamic Waves: I. The Code and Test Cases

1994 ◽  
Vol 144 ◽  
pp. 503-505
Author(s):  
R. Erdélyi ◽  
M. Goossens ◽  
S. Poedts
Keyword(s):  
Resonant Absorption ◽  
Numerical Code ◽  
Mhd Waves ◽  
Test Cases ◽  
Numerical Accuracy ◽  
Element Discretization ◽  
Flux Tubes ◽  
Magnetohydrodynamic Waves ◽  
Viscosity Coefficients ◽  
Magnetic Flux Tubes

AbstractThe stationary state of resonant absorption of linear, MHD waves in cylindrical magnetic flux tubes is studied in viscous, compressible MHD with a numerical code using finite element discretization. The full viscosity tensor with the five viscosity coefficients as given by Braginskii is included in the analysis. Our computations reproduce the absorption rates obtained by Lou in scalar viscous MHD and Goossens and Poedts in resistive MHD, which guarantee the numerical accuracy of the tensorial viscous MHD code.

Structuring, Motions and Shapes of Corona Emission Line Profiles

1994 ◽  
Vol 144 ◽  
pp. 421-426
Author(s):  
N. F. Tyagun
Keyword(s):  
Emission Line ◽  
Filling Factor ◽  
Direct Relationship ◽  
Coronal Plasma ◽  
Line Of Sight ◽  
Line Profiles ◽  
The Difference ◽  
Yellow Line ◽  
Red Line

AbstractThe interrelationship of half-widths and intensities for the red, green and yellow lines is considered. This is a direct relationship for the green and yellow line and an inverse one for the red line. The difference in the relationships of half-widths and intensities for different lines appears to be due to substantially dissimilar structuring and to a set of line-of-sight motions in ”hot“ and ”cold“ corona regions.When diagnosing the coronal plasma, one cannot neglect the filling factor - each line has such a factor of its own.

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