Global Coronal Waves

Chen, P. F.

doi:10.1002/9781119055006.ch22

Cited by 33 publications

(27 citation statements)

References 117 publications

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“…Given the content of Table 2, most of the authors conclude that propagating EIT-wave pulses are most consistent with the fast-mode large-amplitude wave or shock interpretation, while P.F. Chen insists that two types of EUV wave should be distinguished, and only the faster component can be described as a fast-mode wave (Chen, 2016). While there may be stretching of field lines during the CME eruption and/or formation of a current shell with associated Joule heating and/or reconnection between the erupting CME and the surrounding corona, all of these processes would apply to the CME bubble rather than the pulse that is occasionally observed to propagate ahead of it.…”

Section: Discussionmentioning

confidence: 99%

“…This article should be viewed as being complementary to the reviews of EIT waves by Wills-Davey and Attrill (2009), Gallagher and Long (2011), Zhukov (2011), Patsourakos and Vourlidas (2012), Liu and Ofman (2014), and in particular the recent reviews by Warmuth (2015) and Chen (2016). This is achieved by identifying all of the currently measurable properties (and some beyond our current capabilities) for each of the theories or models.…”

Section: Introductionmentioning

confidence: 86%

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Understanding the Physical Nature of Coronal “EIT Waves”

Long¹,

Bloomfield

Chen

et al. 2016

Sol Phys

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For almost 20 years the physical nature of globally propagating waves in the solar corona (commonly called “EIT waves”) has been controversial and subject to debate. Additional theories have been proposed over the years to explain observations that did not agree with the originally proposed fast-mode wave interpretation. However, the incompatibility of observations made using the Extreme-ultraviolet Imaging Telescope (EIT) onboard the Solar and Heliospheric Observatory with the fast-mode wave interpretation was challenged by differing viewpoints from the twin Solar Terrestrial Relations Observatory spacecraft and data with higher spatial and temporal resolution from the Solar Dynamics Observatory. In this article, we reexamine the theories proposed to explain EIT waves to identify measurable properties and behaviours that can be compared to current and future observations. Most of us conclude that the so-called EIT waves are best described as fast-mode large-amplitude waves or shocks that are initially driven by the impulsive expansion of an erupting coronal mass ejection in the low corona.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 86%

Understanding the Physical Nature of Coronal “EIT Waves”

Long¹,

Bloomfield

Chen

et al. 2016

Sol Phys

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“…取了多个名称, 例如极紫外波、全球性日冕波、日冕传播波前、大尺度日冕传播波前等 [3] . 由于EIT波主要是指在极紫外波段被观测到的大尺度扰动现象, 下面将使用大尺度极紫外(extreme-ultraviolet, EUV)波这一…”

Section: Eit波的观测大致可分为3个阶段分别以Sohounclassified

“…但是, 如果考虑所有EUV波, 它与射电II型暴之间的相关性却不高 [28,69~71] . 这可能是由于统计样本中包含了大量慢速的表观波动事例 [3] ; 另外, 可能还有许多是线性或简单波, 它们并未形成激波进而造成射电II型暴, 或是激波强度不足以产生射电辐射.…”

Section: 对它们的驱动时间长短不同所造成径向部分被Cmeunclassified

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Research progress on coronal extreme ultraviolet waves

Shen¹,

Li²,

Chen³

et al. 2020

Chin. Sci. Bull.

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Comparison of the coronal mass ejection shock acceleration of three widespread SEP events during solar cycle 24

et al. 2017

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We studied three solar energetic particle (SEP) events observed on 14 August 2010, 3 November 2011, and 5 March 2013 by Solar Terrestrial Relations Observatory (STEREO) A, B, and near‐Earth (L1) spacecraft with a longitudinal distribution of particles >90°. Using a forward modeling method combined with extreme ultraviolet and white‐light images, we determined the angular extent of the shock, the time and location (cobpoint) of the shock intersection with the magnetic field line connecting to each spacecraft, and compute the shock speed at the cobpoint of each spacecraft. We then examine whether the observations of SEPs at each spacecraft were accelerated and injected by the spatially extended shocks or whether another mechanism such as cross‐field transport is required for an alternative explanation. Our analyses results indicate that the SEPs observed at the three spacecraft on 3 November, STEREO B (STB) and L1 on 14 August, and the 5 March SEP event at STEREO A (STA) can be explained by the direct shock acceleration. This is consistent with the observed significant anisotropies, short time delays between particle release times and magnetic connection times, and sharp rises in the SEP time profiles. Cross‐field diffusion is the likely cause for the 14 August SEP event observed by STA and the 5 March SEPs observed by STB and L1 spacecraft, as particle observations featured weak electron aniotropies and slow rising intensity profiles. Otherwise, the wide longitudinal spread of these SEP increases would require an existence of a circumsolar shock, which may not be a correct assumption in the corona and heliosphere.

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Global Coronal Waves

Cited by 33 publications

References 117 publications

Understanding the Physical Nature of Coronal “EIT Waves”

Understanding the Physical Nature of Coronal “EIT Waves”

Research progress on coronal extreme ultraviolet waves

Comparison of the coronal mass ejection shock acceleration of three widespread SEP events during solar cycle 24

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