Observations and Interpretation of a Low Coronal Shock Wave Observed in the Euv by the Sdo/Aia

Ma, Suli; Raymond, J. C.; Golub, L.; Lin, Jin‐Ming; Chen, Huadong; Grigis, P. C.; Testa, Paola; Long, David M.

doi:10.1088/0004-637x/738/2/160

Cited by 164 publications

(213 citation statements)

References 66 publications

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“…This correlation could not be established for EIT wave speeds (Klassen et al, 2000), most likely due to the severe undersampling of the waves' kinematics. A kinematical consistency (in terms of distances/heights and speeds) between type II bursts and coronal waves was also found in a large number of case studies (e.g., Vršnak et al, 2006;Pohjolainen et al, 2008;Grechnev et al, 2011b,a;Kozarev et al, 2011;Ma et al, 2011;Kumar and Manoharan, 2013). An example is shown in the right panel of Figure 15.…”

Section: Metric Type II Radio Burstssupporting

confidence: 56%

“…They found that the type II burst kinematics were consistent with the wave and that the wave itself was consistent with a weak shock (Kozarev et al, 2011;Ma et al, 2011). The compression ratios derived from the band-split of the type II burst and from the EUV imaging data are actually consistent ( ≈ 1.5) and decline during the wave's propagation (Kouloumvakos et al, 2014).…”

Section: Metric Type II Radio Burstsmentioning

confidence: 90%

“…In limb events, fast wavelike fronts were clearly observed to decouple from CME-associated fronts which are significantly slower or even come to a halt (e.g., Kienreich et al, 2009;Ma et al, 2011;Chen and Wu, 2011;Dai et al, 2012). This will be discussed in more detail in Section 5.2.…”

Section: Multiple Wavefrontsmentioning

confidence: 92%

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Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

163

140

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Large-scale, globally propagating wave-like disturbances have been observed in the solar chromosphere and by inference in the corona since the 1960s. However, detailed analysis of these phenomena has only been conducted since the late 1990s. This was prompted by the availability of high-cadence coronal imaging data from numerous spaced-based instruments, which routinely show spectacular globally propagating bright fronts. Coronal waves, as these perturbations are usually referred to, have now been observed in a wide range of spectral channels, yielding a wealth of information. Many findings have supported the "classical" interpretation of the disturbances: fast-mode MHD waves or shocks that are propagating in the solar corona. However, observations that seemed inconsistent with this picture have stimulated the development of alternative models in which "pseudo waves" are generated by magnetic reconfiguration in the framework of an expanding coronal mass ejection. This has resulted in a vigorous debate on the physical nature of these disturbances. This review focuses on demonstrating how the numerous observational findings of the last one and a half decades can be used to constrain our models of large-scale coronal waves, and how a coherent physical understanding of these disturbances is finally emerging. Article RevisionsLiving Reviews supports two ways of keeping its articles up-to-date:Fast-track revision. A fast-track revision provides the author with the opportunity to add short notices of current research results, trends and developments, or important publications to the article. A fast-track revision is refereed by the responsible subject editor. If an article has undergone a fast-track revision, a summary of changes will be listed here.Major update. A major update will include substantial changes and additions and is subject to full external refereeing. It is published with a new publication number.For detailed documentation of an article's evolution, please refer to the history document of the article's online version at http://dx

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Section: Metric Type II Radio Burstssupporting

confidence: 56%

Section: Metric Type II Radio Burstsmentioning

confidence: 90%

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Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

163

140

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“…Recent observations have provided convincing evidence that shocks can form and accelerate particles low in the corona. Ma et al (2011) suggested that the brightness enhancement ahead of the bright CME front seen by extreme ultraviolet observations of SDO/AIA is a shock signature and it forms as low as ∼1.2 R e from the center of the Sun. Gopalswamy et al (2013b) found that CME shock formation can occur substantially below ∼1.5 R e from observations of type II radio bursts produced by electrons accelerated by shocks.…”

Section: Introductionmentioning

confidence: 99%

The Acceleration of High-energy Protons at Coronal Shocks: The Effect of Large-scale Streamer-like Magnetic Field Structures

Kong

Guo

Giacalone

et al. 2017

ApJ

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Recent observations have shown that coronal shocks driven by coronal mass ejections can develop and accelerate particles within several solar radii in large solar energetic particle (SEP) events. Motivated by this, we present an SEP acceleration study that including the process in which a fast shock propagates through a streamer-like magnetic field with both closed and open field lines in the low corona region. The acceleration of protons is modeled by numerically solving the Parker transport equation with spatial diffusion both along and across the magnetic field. We show that particles can be sufficiently accelerated to up to several hundred MeV within 2-3 solar radii. When the shock propagates through a streamer-like magnetic field, particles are more efficiently accelerated compared to the case with a simple radial magnetic field, mainly due to perpendicular shock geometry and the natural trapping effect of closed magnetic fields. Our results suggest that the coronal magnetic field configuration is an important factor for producing large SEP events. We further show that the coronal magnetic field configuration strongly influences the distribution of energetic particles, leading to different locations of source regions along the shock front where most high-energy particles are concentrated. This work may have strong implications for SEP observations. The upcoming Parker Solar Probe will provide in situ observations for the distribution of energetic particles in the coronal shock region, and test the results of the study.

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“…As seen from Figures 2 and 3, the EUV wave appeared as bright tracks in the hotter 193, 211 and 335Å channels, while a dark track in the cooler 171Å channel, suggesting plasma heating (Wills-Davey & Thompson 1999;Liu et al 2010Liu et al , 2012Long et al 2011a;Ma et al 2011;Li et al 2012). In the 211 channel, the average propagation velocities of this EUV wave were from (448±9) to (900±10) km s −1 in the three directions.…”

Section: Observations and Data Analysismentioning

confidence: 84%

SDO/AIA and Hinode/EIS observations of interaction between an EUV wave and active region loops

Liu¹,

Zhang²,

Li³

et al. 2012

Proc. IAU

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We present detailed analysis of an extreme ultraviolet (EUV) wave and its interaction with active region (AR) loops observed by the Solar Dynamics Observatory/Atmospheric Imaging Assembly and the Hinode EUV Imaging Spectrometer (EIS). This wave was initiated from AR 11261 on 2011 August 4 and propagated at velocities of 430-910 km s −1 . It was observed to traverse another AR and cross over a filament channel on its path. The EUV wave perturbed neighboring AR loops and excited a disturbance that propagated toward the footpoints of these loops. EIS observations of AR loops revealed that at the time of the wave transit, the original redshift increased by about 3 km s −1 , while the original blueshift decreased slightly. After the wave transit, these changes were reversed. When the EUV wave arrived at the boundary of a polar coronal hole, two reflected waves were successively produced and part of them propagated above the solar limb. The first reflected wave above the solar limb encountered a large-scale loop system on its path, and a secondary wave rapidly emerged 144 Mm ahead of it at a higher speed. These findings can be explained in the framework of a fast-mode magnetosonic wave interpretation for EUV waves, in which observed EUV waves are generated by expanding coronal mass ejections.

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Observations and Interpretation of a Low Coronal Shock Wave Observed in the Euv by the Sdo/Aia

Cited by 164 publications

References 66 publications

Large-scale Globally Propagating Coronal Waves

Large-scale Globally Propagating Coronal Waves

The Acceleration of High-energy Protons at Coronal Shocks: The Effect of Large-scale Streamer-like Magnetic Field Structures

SDO/AIA and Hinode/EIS observations of interaction between an EUV wave and active region loops

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