Special Issue "Solar Coronal Waves and Their Imprints in the Lower Atmosphere"
Deadline for manuscript submissions: 31 December 2022 | Viewed by 49
Interests: physics of solar eruptions; physics of the solar corona
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Solar coronal waves are impressive propagating disturbances that are best seen as enhancements in the intensity of extreme ultraviolet emission. Coronal waves can be associated with large-scale coronal mass ejections and flares and small-scale jets, and have been interpreted in the model of true magnetohydrodynamic (MHD) waves, pseudo-waves, or hybrid waves. Before the observational discovery of coronal waves, their existence was predicted by the detection of chromospheric Moreton waves in the 1960s. Moreton waves are interpreted as ground tracks of coronal fast-mode MHD wavefronts that sweep over the chromosphere.
Hundreds of coronal waves have been found and studied, but the number of detective chromospheric Moreton waves is limited. As the origin of chromospheric Moreton waves, why did most coronal waves fail to ignite a detectable chromospheric disturbance? On the other hand, if the coronal wave can successfully compress the chromosphere, the transient region (TR) as an interface between them should be compressed first; however, wave signatures in TR are also rarely reported.
The proposed Special Issue seeks to gather new results on solar coronal waves and their imprints on the lower atmosphere, and aims to provide a platform for scientists around the world to better understand the physical nature and driving mechanisms of solar coronal waves.
Prof. Dr. Ruisheng Zheng
Manuscript Submission Information
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- solar eruptions
- coronal waves
- Moreton waves
- coronal mass ejections (CMEs)
- solar flares
- solar jets