PLASMA DIAGNOSTICS OF AN EIT WAVE OBSERVED BY
                    <i>HINODE</i>
                    /EIS AND
                    <i>SDO</i>
                    /AIA

Veronig, Astrid; Gömöry, P.; Kienreich, I. W.; Muhr, N.; Vršnak, Bojan; Temmer, Manuela; Warren, H. P.

doi:10.1088/2041-8205/743/1/l10

Cited by 50 publications

(58 citation statements)

References 35 publications

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“…The downward motion is caused by the downward push of the CME during its expansion into the corona. This same phenomenon was observed to occur in AR 11158 by Harra et al (2011) and Veronig et al (2011) using data from the Hinode/EUV imaging spectrometer (Culhane et al 2007) during an M1.6 flare/CME event on 2011 February 16. The upward motion is induced by the radial propagation of the CME and is more often observed in the Dopplergrams after CMEs (e.g., Harra et al 2007;Imada et al 2007;Jin et al 2009;Tian et al 2012).…”

Section: Dynamic Evolution After the Eruptionsupporting

confidence: 68%

A Numerical Study of Long-Range Magnetic Impacts During Coronal Mass Ejections

Jin

Schrijver

Cheung

et al. 2016

ApJ

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With the global view and high-cadence observations from Solar Dynamics Observatory/Atmospheric Imaging Assembly and Solar TErrestrial RElations Observatory, many spatially separated solar eruptive events appear to be coupled. However, the mechanisms for "sympathetic" events are still largely unknown. In this study, we investigate the impact of an erupting flux rope on surrounding solar structures through large-scale magnetic coupling. We build a realistic environment of the solar corona on 2011 February 15 using a global magnetohydrodynamics model and initiate coronal mass ejections (CMEs) in active region 11158 by inserting Gibson-Low analytical flux ropes. We show that a CME's impact on the surrounding structures depends not only on the magnetic strength of these structures and their distance to the source region, but also on the interaction between the CME and the large-scale magnetic field. Within the CME expansion domain where the flux rope field directly interacts with the solar structures, expansion-induced reconnection often modifies the overlying field, thereby increasing the decay index. This effect may provide a primary coupling mechanism underlying the sympathetic eruptions. The magnitude of the impact is found to depend on the orientation of the erupting flux rope, with the largest impacts occurring when the flux rope is favorably oriented for reconnecting with the surrounding regions. Outside the CME expansion domain, the influence of the CME is mainly through field line compression or post-eruption relaxation. Based on our numerical experiments, we discuss a way to quantify the eruption impact, which could be useful for forecasting purposes.

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Section: Dynamic Evolution After the Eruptionsupporting

confidence: 68%

A Numerical Study of Long-Range Magnetic Impacts During Coronal Mass Ejections

Jin

Schrijver

Cheung

et al. 2016

ApJ

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“…After the wave transit, these changes were reversed. Our results are similar to the recent studies using Hinode/EIS and SDO/AIA observations Veronig et al 2011). It can be explained by the scenario of a fast-mode wave model as described by Uchida (1968).…”

Section: Conclusion and Discussionsupporting

confidence: 92%

“…The plasma density decreased by about 2.9×10 8 cm −3 in "A" and 1.1×10 8 cm −3 in "B", which were within the variation range of the plasma density between 02:07 and 03:08 UT. These observational results were similar to those given by Veronig et al (2011), in which small density changes associated with an EUV wave. We note that after the EUV wave transit, the plasma density reached a peak of 1.8×10 10 cm −3 in "B" and of 9.1×10 9 cm −3 in "A" , marked by "dp2" and "dp1", respectively.…”

Section: Spectroscopic Analysis Of the Euv Wavesupporting

confidence: 91%

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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“…In this weak event, little or no line-of-sight motions could be detected in the CDS spectra ( ≤ 10 km s -1 ). The first clear detection of flows in an EUV wave were made with Hinode/EIS by Harra et al (2011) and Veronig et al (2011). In this event, the usual blueshifts associated with the upflows in dimmings are seen close to the source AR.…”

Section: Flowsmentioning

confidence: 95%

“…Unambiguous values for can only be obtained from spectroscopic observations of density-sensitive EUV or SXR lines. Unfortunately there has been only one such observations up to now: Veronig et al (2011) used Hinode/EIS observations of the Fe xiii 202/203Å line pair to deduce ≤ 1.1 in one coronal wave event (see also Section 4.6). This was within the noise limit of EIS, so more spectroscopic observations would be highly desirable.…”

Section: Perturbation Profilementioning

confidence: 99%

Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

154

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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PLASMA DIAGNOSTICS OF AN EIT WAVE OBSERVED BY HINODE /EIS AND SDO /AIA

Cited by 50 publications

References 35 publications

A Numerical Study of Long-Range Magnetic Impacts During Coronal Mass Ejections

A Numerical Study of Long-Range Magnetic Impacts During Coronal Mass Ejections

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

Large-scale Globally Propagating Coronal Waves

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