Propagation of a global coronal wave and its interaction with large-scale coronal magnetic structures

Context. Global coronal waves associated with solar eruptions (the so-called EIT waves) often encounter coronal holes and solar active regions and interact with these magnetic structures. This interaction leads to a number of observed effects such as wave reflection and transmission. Aims. We consider the propagation of a large-scale coronal shock wave and its interaction with large-scale non-uniformities of the background magnetic field and plasma parameters. Methods. Using the Lare2d code, we performed 2.5-dimensional simulations of the interaction of a large-scale single-pulse fast-mode magnetohydrodynamic shock wave of weak-to-moderate intensity with the region of enhanced Alfvén speed as well as with that of reduced Alfvén speed. We analysed simple models of non-uniformity and the surrounding plasma to understand the basic effects in wave propagation. Results. We found the reflected waves of plasma compression and rarefaction, transmitted waves that propagate behind or ahead of the main part of the wave, depending on properties of the plasma non-uniformity, and secondary wave fronts. The obtained results are important to the correct interpretation of the global coronal wave propagation in the solar corona, understanding of theoretical aspects of the interaction of large-scale coronal shock waves with large-scale coronal magnetic structures, and diagnostics of coronal plasma parameters.

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HelioSwarm: The Nature of Turbulence in Space Plasmas

10.5194/egusphere-egu21-12092 ◽

2021 ◽

Author(s):

Harlan Spence ◽

Kristopher Klein ◽

HelioSwarm Science Team

Keyword(s):

Magnetic Field ◽

Solar Wind ◽

Large Scale ◽

Solar Wind Plasma ◽

Turbulent Energy ◽

Space Plasmas ◽

Plasma Parameters ◽

Astrophysical Plasmas ◽

Ion Distributions ◽

Background Magnetic Field

<p>Recently selected for phase A study for NASA&#8217;s Heliophysics MidEx Announcement of Opportunity, the HelioSwarm Observatory proposes to transform our understanding of the physics of turbulence in space and astrophysical plasmas by deploying nine spacecraft to measure the local plasma and magnetic field conditions at many points, with separations between the spacecraft spanning MHD and ion scales.&#160;&#160;HelioSwarm resolves the transfer and dissipation of turbulent energy in weakly-collisional magnetized plasmas with a novel configuration of spacecraft in the solar wind. These simultaneous multi-point, multi-scale measurements of space plasmas allow us to reach closure on two science goals comprised of six science objectives: (1) reveal how turbulent energy is transferred in the most probable, undisturbed solar wind plasma and distributed as a function of scale and time; (2) reveal how this turbulent cascade of energy varies with the background magnetic field and plasma parameters in more extreme solar wind environments; (3) quantify the transfer of turbulent energy between fields, flows, and ion heat; (4) identify thermodynamic impacts of intermittent structures on ion distributions; (5) determine how solar wind turbulence affects and is affected by large-scale solar wind structures; and (6) determine how strongly driven turbulence differs from that in the undisturbed solar wind.&#160;</p>

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Multi-wavelength observations of filament oscillations induced by shock waves

Proceedings of the International Astronomical Union ◽

10.1017/s1743921316000193 ◽

2015 ◽

Vol 11 (S320) ◽

pp. 106-108

Author(s):

Yuandeng Shen

Keyword(s):

Shock Wave ◽

Magnetic Fields ◽

Shock Waves ◽

Large Scale ◽

Coronal Shock ◽

First Case ◽

Proper Order ◽

Multi Wavelength ◽

Limb Prominence ◽

A Chain

AbstractTwo cases of filament oscillations induced by large-scale coronal shock waves are presented. For the first case, a chain of transverse oscillating filaments are observed in a proper order after the passing of a shock wave, and it is found that the they were triggered by the surface component of the dome-shaped shock wave. For the second case, simultaneous transverse oscillation of a limb prominence and longitudinal oscillation in an on-disk filament are launched by a single shock wave. It is found that the interaction angle between the shock wave and the prominence axis is the key to launch transverse or longitudinal filament oscillations. In addition, filament magnetic fields are estimated, using the measured parameters.

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Coronal Shock Waves, EUV Waves, and Their Relation to CMEs. II. Modeling MHD Shock Wave Propagation Along the Solar Surface, Using Nonlinear Geometrical Acoustics

Solar Physics ◽

10.1007/s11207-011-9730-9 ◽

2011 ◽

Vol 273 (2) ◽

pp. 479-491 ◽

Cited By ~ 24

Author(s):

A. N. Afanasyev ◽

A. M. Uralov

Keyword(s):

Shock Wave ◽

Wave Propagation ◽

Shock Waves ◽

Solar Surface ◽

Shock Wave Propagation ◽

Coronal Shock ◽

Geometrical Acoustics

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Shock wave propagation, plasticity, and void collapse in open-cell nanoporous Ta

Physical Chemistry Chemical Physics ◽

10.1039/c8cp05126g ◽

2018 ◽

Vol 20 (44) ◽

pp. 28039-28048 ◽

Cited By ~ 6

Author(s):

J. F. Tang ◽

J. C. Xiao ◽

L. Deng ◽

W. Li ◽

X. M. Zhang ◽

...

Keyword(s):

Shock Wave ◽

Molecular Dynamics ◽

Wave Propagation ◽

Specific Surface ◽

Molecular Dynamics Simulations ◽

Surface Area ◽

Large Scale ◽

Open Cell ◽

Non Equilibrium Molecular Dynamics ◽

Dynamics Simulations

We systematically investigate the wave propagation, plasticity and void collapse, as well as the effects of porosity, specific surface area and impact velocity, in a set of open-cell nanoporous Ta, during shock compression, via performing large-scale non-equilibrium molecular dynamics simulations.

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