EUVI: the STEREO-SECCHI extreme ultraviolet imager

Wüelser, Jean-Pierre; Lemen, J. R.; Tarbell, T. D.; Wolfson, C. J.; Cannon, Joseph C.; Carpenter, Brock A.; Duncan, D.; Gradwohl, Glenn S.; Meyer, S.; Moore, Augustus S.; Navarro, Rosemarie L.; Pearson, J. D.; Rossi, G.; Springer, Larry; Howard, R. A.; Moses, J. D.; Newmark, Jeffrey; Delaboudinière, J. P.; Artzner, G.; Auchère, F.; Bougnet, M.; Bouyries, Philippe; Bridou, Françoise; Clotaire, Jean-Yves; Colas, Gerard; Delmotte, Franck; Adnot, Jérôme; Lamare, Michel; Mercier, Raymond; Mullot, Michel; Ravet, M. F.; Song, Xueyan; Bothmer, V.; Deutsch, W.

doi:10.1117/12.506877

Cited by 449 publications

(106 citation statements)

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“…The proposed GPU-accelerated DBIE is applied to reconstruct the coronal magnetic field from the vector magnetogram taken on 2011 February 14 at 20:12 UT from SDO/HMI. This is combined with observations from the SDO/AIA and the two STEREO/Extreme Ultraviolet Imager (EUVI) instruments (Howard et al, 2008;Wülser et al, 2004) to present a stereoscopic investigation of the coronal magnetic fields in order to understand the X2.2 flare event. We average the boundary data from 360 km pix −1 (0.5 ) to 720 km pix −1 (about 1 ), which has 300 × 300 grid points to be used as the boundary condition.…”

Section: Observationsmentioning

confidence: 99%

Three-Dimensional Nonlinear Force-Free Field Reconstruction of Solar Active Region 11158 by Direct Boundary Integral Equation

2013

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A 3-D coronal magnetic field is reconstructed for the NOAA active region 11158 on February 14, 2011. A GPU-accelerated direct boundary integral equation (DBIE) method is implemented. This is approximately 1000 times faster than the original DBIE used on solar non-linear force-free field modeling. Using the SDO/HMI vector magnetogram as the bottom boundary condition, the reconstructed magnetic field lines are compared with the projected EUV loop structures as observed by SDO/AIA at front view and the STEREO A/B spacecraft at side views for the first time. They show very good agreement three-dimensionally so that the topology configurations of the magnetic fields can be analyzed, thus its role in the flare process of the active region can be better understood. A quantitative comparison with some stereoscopically reconstructed coronal loops shows that the present averaged misalignment angles are at the same order as the state-of-the-art results obtained with reconstructed coronal loops as prescribed conditions. It is found that the observed coronal loop structures can be grouped into a number of closed and open field structures with some central bright coronal loop features around the polarity inversion line. The reconstructed highly-shearing magnetic field lines agree very well with the low-lying sigmoidal filament along the polarity inversion line. They are in a pivot position to all other surrounding coronal structures, and a group of electric current lines co-aligned with the central bright EUV loops overlying the filament channel is also obtained. This central lower-lying magnetic field loop system must have played a key role in powering the flare. It should be noted that while a strand-like coronal feature along the polarity inversion line may be related to the filament, one cannot simply attribute all the coronal bright features along the polarity inversion line to manifestation of the filament without any stereoscopical information. The numerical procedure and the comparison against a benchmark test case are also presented to validate that the DBIE method is rigorous and effective.

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Section: Observationsmentioning

confidence: 99%

Three-Dimensional Nonlinear Force-Free Field Reconstruction of Solar Active Region 11158 by Direct Boundary Integral Equation

2013

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“…We like to close this section, pointing out an unconventional work, based on SOHO/EIT and STEREO/EUVI (Wülser et al, 2004) data, made by de Patoul et al (2013a), who, starting from the plume orientation and assuming that the magnetic field of the Sun changes slowly with respect to the solar rotation rate, developed a procedure to calculate the temporal evolution of the magnetic poles of the Sun. Because the orientation of the plumes changes when new magnetic flux emerges, in an interesting future application of this research, we might be able to probe indirectly the flux emergence on the far side of the Sun, via observations of the inclination of plumes and of flux emergence in the visible side of the Sun.…”

Section: Introductionmentioning

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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“…Significant progress has resulted from the high-cadence EUV imaging that has become available with the Extreme Ultraviolet Imager (EUVI; Wülser et al, 2004;Howard et al, 2008) on the two STEREO spacecraft, the Sun Watcher using Active Pixel detectors and Image Processing (SWAP; Halain et al, 2010) aboard PROBA2, and the Atmospheric Imaging Assembly (AIA; Lemen et al, 2012) aboard SDO. These instruments have provided a wealth of observational data, so that the EUV spectral range is now clearly the most important spectral range with respect to coronal waves.…”

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confidence: 99%

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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EUVI: the STEREO-SECCHI extreme ultraviolet imager

Cited by 449 publications

References 5 publications

Three-Dimensional Nonlinear Force-Free Field Reconstruction of Solar Active Region 11158 by Direct Boundary Integral Equation

Three-Dimensional Nonlinear Force-Free Field Reconstruction of Solar Active Region 11158 by Direct Boundary Integral Equation

Solar Coronal Plumes

Large-scale Globally Propagating Coronal Waves

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