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

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 Modeling Prominence Formation in 2.5D

2013 ◽  
Vol 8 (S300) ◽  
pp. 410-411
Author(s):  
X. Fang ◽  
C. Xia ◽  
R. Keppens
Keyword(s):  
Numerical Simulations ◽  
Transition Region ◽  
Formation Process ◽  
Coronal Plasma ◽  
Fixed Angle ◽  
Spatial Range ◽  
Normal Polarity ◽  
Linear Force ◽  
Magnetic Arcade ◽  
Chromospheric Heating

AbstractWe use a 2.5-dimensional, fully thermodynamically and magnetohydrodynamically compatible model to imitate the formation process of normal polarity prominences on top of initially linear force-free arcades above photospheric neutral lines. In magnetic arcades hosting chromospheric, transition region, and coronal plasma, we perform a series of numerical simulations to do a parameter survey for multi-dimensional evaporation-condensation prominence models. The investigated parameters include the fixed angle of the magnetic arcade, the strength and spatial range of the localized chromospheric heating.

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

Numerical simulations of driven MHD waves in coronal loops

Solar Physics ◽  
1996 ◽  
Vol 167 (1-2) ◽  
pp. 181-202 ◽  
Author(s):  
S. Parhi ◽  
P. De Bruyne ◽  
K. Murawski ◽  
M. Goossens ◽  
C. R. Devore
Keyword(s):  
Numerical Simulations ◽  
Mhd Waves ◽  
Coronal Loops

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

scholarly journals Comparison of numerical simulations and observations of helioseismic MHD waves in sunspots

2010 ◽  
Vol 6 (S273) ◽  
pp. 422-425
Author(s):  
K. V. Parchevsky ◽  
J. Zhao ◽  
A. G. Kosovichev ◽  
M. Rempel
Keyword(s):  
Numerical Simulations ◽  
Time Lag ◽  
Initial Step ◽  
Wave Transformation ◽  
Mhd Waves ◽  
Multiple Sources ◽  
Localized Source ◽  
Covariance Functions ◽  
Cross Covariance ◽  
The Magnetic Field

AbstractNumerical 3D simulations of MHD waves in magnetized regions with background flows are very important for the understanding of propagation and transformation of waves in sunspots. Such simulations provide artificial data for testing and calibration of helioseismic techniques used for analysis of data from space missions SOHO/MDI, SDO/HMI, and HINODE. We compare with helioseismic observations results of numerical simulations of MHD waves in different models of sunspots. The simulations of waves excited by a localized source provide a detailed picture of the interaction of the MHD waves with the magnetic field and background flows (deformation of the waveform, wave transformation, amplitude variations and anisotropy). The observed cross-covariance function represents an effective Green's function of helioseismic waves. As an initial step, we compare it with simulations of waves generated by a localized source. More thorough analysis implies using multiple sources and comparison of the observed and simulated cross-covariance functions. We plan to do such calculations in the nearest future. Both, the simulations and observations show that the wavefront inside the sunspot travels ahead of a reference “quiet Sun” wavefront, when the wave enters the sunspot. However, when the wave passes the sunspot, the time lag between the wavefronts becomes unnoticeable.

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