EIT Observations of the Extreme Ultraviolet Sun

Moses, D.; Clette, F.; Delaboudinière, J.-P.; Artzner, G.; Bougnet, M.; Brunaud, J.; Carabetian, C.; Gabriel, A. H.; Hochedez, Jean-François; Millier, F.; Song, Xueyan; Au, B.; Dere, K. P.; Howard, R. A.; Kreplin, R. W.; Michels, D. J.; Defise, Jean-Marc; Jamar, C.; Rochus, Pierre; Chauvineau, J.P.; Marioge, J P; Catura, R. C.; Lemen, J. R.; Shing, L.; Stern, Robert; Gurman, J. B.; Neupert, W. M.; Newmark, J. S.; Thompson, B. J.; Maucherat, A.; Portier-Fozzani, F.; Berghmans, David; Cugnon, P.; Dessel, E. L. van; Gabryl, J. R.

doi:10.1007/978-94-011-5236-5_32

Cited by 26 publications

(27 citation statements)

References 21 publications

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“…These postulated coronal disturbances were finally observed in 1997 with the Extreme Ultraviolet Imaging Telescope (EIT; Delaboudinière et al, 1995) aboard the SOHO spacecraft. They take the form of spectacular wave-like features propagating globally through the corona (Moses et al, 1997;.…”

Section: Overviewmentioning

confidence: 99%

“…4 These disturbances have become known as EIT waves and are primarily observed at 195Å (which is dominated by line emission of the Fe xii ion, corresponding to a plasma temperature of 1.4 MK). The perturbations take the form of moving fronts of increased EUV emission that propagate quasi-radially away from active regions at speeds of typically a few 100 km s -1 (Moses et al, 1997;Thompson et al, , 1999 Figure 3 and the animation in Figure 4 for a "textbook example"). The observed pulses are usually quite faint (emission increase below ≈ 25%) and diffuse, can have an angular extent up to 360°, and can propagate over a whole hemisphere (to distances beyond one solar radius).…”

Section: Extreme Ultraviolet (Euv)mentioning

confidence: 99%

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Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

169

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: Overviewmentioning

confidence: 99%

Section: Extreme Ultraviolet (Euv)mentioning

confidence: 99%

Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

169

140

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“…A method quite analogous to that used by Ahmad and Withbroe (1977) has been adopted by, e.g., DeForest et al (1997) and Moses et al (1997), who, from the ratio of the intensities of plumes imaged by SOHO/EIT in the 171 (Fe ix/x) and 195 (Fe xii) channels, derived temperatures in the range 1 -1.5 MK. Figure 4 shows images of plumes acquired by the SOHO/EIT telescope in two wave bands, the 171 Fe ix/x and the Fe xii 195Å with peak sensitivities, respectively, at ≈ 1 MK and 1.5 MK.…”

Section: Densities and Temperatures Of Plumes From Xuv Datamentioning

confidence: 99%

“…In the late 1990s, Moses et al (1997) described UV jets in polar CHs and shortly afterwards Lites et al (1999) from WL and EIT data, detected a jet embedded in a polar plume propagating upwards at a speed of ≈ 200 km s -1 . About a decade later, addressed the issue of the relationship, if any, between plumes and X-ray jets.…”

Section: The Birth Of Plumesmentioning

confidence: 99%

Solar Coronal Plumes

Poletto

2015

Living Rev. Sol. Phys.

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Polar plumes are thin long ray-like structures that project beyond the limb of the Sun polar regions, maintaining their identity over distances of several solar radii. Plumes have been first observed in white-light (WL) images of the Sun, but, with the advent of the space era, they have been identified also in X-ray and UV wavelengths (XUV) and, possibly, even in in situ data. This review traces the history of plumes, from the time they have been first imaged, to the complex means by which nowadays we attempt to reconstruct their 3-D structure. Spectroscopic techniques allowed us also to infer the physical parameters of plumes and estimate their electron and kinetic temperatures and their densities. However, perhaps the most interesting problem we need to solve is the role they cover in the solar wind origin and acceleration: Does the solar wind emanate from plumes or from the ambient coronal hole wherein they are embedded? Do plumes have a role in solar wind acceleration and mass loading? Answers to these questions are still somewhat ambiguous and theoretical modeling does not provide definite answers either. Recent data, with an unprecedented high spatial and temporal resolution, provide new information on the fine structure of plumes, their temporal evolution and relationship with other transient phenomena that may shed further light on these elusive features. 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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“…Initially identified as fast-mode MHD waves (e.g. Dere et al, 1997;Moses et al, 1997;Thompson et al, 1998), this interpretation was questioned following observations of stationary bright fronts at coronal hole boundaries and anomalously low measured kinematics (cf. Delannée and Aulanier, 1999).…”

Section: Introductionmentioning

confidence: 99%

A Statistical Analysis of the Solar Phenomena Associated with Global EUV Waves

et al. 2017

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Solar eruptions are the most spectacular events in our solar system and are associated with many different signatures of energy release including solar flares, coronal mass ejections, global waves, radio emission and accelerated particles. Here, we apply the Coronal Pulse Identification and Tracking Algorithm (CorPITA) to the high-cadence synoptic data provided by the Solar Dynamics Observatory (SDO) to identify and track global waves observed by SDO. 164 of the 362 solar flare events studied (45%) were found to have associated global waves with no waves found for the remaining 198 (55%). A clear linear relationship was found between the median initial velocity and the acceleration of the waves, with faster waves exhibiting a stronger deceleration (consistent with previous results). No clear relationship was found between global waves and type II radio bursts, electrons or protons detected in situ near Earth. While no relationship was found between the wave properties and the associated flare size (with waves produced by flares from B to X-class), more than a quarter of the active regions studied were found to produce more than one wave event. These results suggest that the presence of a global wave in a solar eruption is most likely determined by the structure and connectivity of the erupting active region and the surrounding quiet solar corona rather than by the amount of free energy available within the active region.

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EIT Observations of the Extreme Ultraviolet Sun

Cited by 26 publications

References 21 publications

Large-scale Globally Propagating Coronal Waves

Large-scale Globally Propagating Coronal Waves

Solar Coronal Plumes

A Statistical Analysis of the Solar Phenomena Associated with Global EUV Waves

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