Special Issue "Extreme Ultraviolet Waves in Solar Corona"

A special issue of Galaxies (ISSN 2075-4434).

Deadline for manuscript submissions: closed (18 February 2022) | Viewed by 1187

Special Issue Editor

Prof. Dr. Ruisheng Zheng
E-Mail Website
Guest Editor
School of Space Science and Physics, Shandong University, Weihai 264209, China
Interests: physics of solar eruptions; physics of the solar corona
Special Issues, Collections and Topics in MDPI journals

Special Issue Information

Dear Colleagues,

Extreme ultraviolet (EUV) waves are impressive coronal propagating disturbances that are best seen as intensity enhancements in EUV emission. EUV waves are also called “EIT waves”, “coronal bright fronts”, and “large-scale coronal propagating fronts”. EUV waves can provide potential diagnostics on coronal magnetic field strengths and coronal plasma parameters. Since the discovery of the first case, the EUV wave has been strongly debated in relation to the physical nature of a true wave or a pseudo wave. On the other hand, it is widely recognized that EUV waves are always associated with a variety of energetic eruptions, such as CMEs, flares, and filament eruptions. Benefiting from high resolution observations from the Solar Terrestrial Relations Observatory (STEREO) and the Solar Dynamics Observatory (SDO), an increasing number of EUV waves are being easily captured, including many small-scale cases that are associated with weak eruptions and present many new observational characteristics.

The proposed issue is scheduled for gathering new results of EUV waves in solar corona and aims to pave the way for better understanding the physical nature and driving mechanisms of solar EUV waves.

Prof. Dr. Ruisheng Zheng
Guest Editor

Manuscript Submission Information

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Keywords

  • extreme ultraviolet
  • EIT waves
  • solar corona

Published Papers (1 paper)

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Research

Article
Dynamics and Kinematics of the EUV Wave Event on 6 May 2019
Galaxies 2022, 10(2), 58; https://doi.org/10.3390/galaxies10020058 - 10 Apr 2022
Viewed by 769
Abstract
We present here the kinematics of the EUV wave associated with a GOES M1.0-class solar flare, which originates in NOAA AR 12740. The event is thoroughly observed with Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO) with high spatio-temporal resolutions. This event [...] Read more.
We present here the kinematics of the EUV wave associated with a GOES M1.0-class solar flare, which originates in NOAA AR 12740. The event is thoroughly observed with Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO) with high spatio-temporal resolutions. This event displays many features of EUV waves, which are very decisive for the understanding of the nature of EUV waves. These features include: a fast-mode wave, a pseudo wave, a slow-mode wave and stationary fronts, probably due to mode conversion. One fast-mode wave also propagates towards the coronal hole situated close to the north pole and the wave speed does not change when it encounters the coronal hole. We intend to provide self-consistent interpretations for all these different features. Full article
(This article belongs to the Special Issue Extreme Ultraviolet Waves in Solar Corona)
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