The Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO)

Lemen, J. R.; Title, A. M.; Akin, D. J.; Boerner, P.; Chou, Cathy; Drake, J. F.; Duncan, D.; Edwards, Christopher G.; Friedlaender, Frank M.; Heyman, Gary F.; Hurlburt, N. E.; Katz, N.; Kushner, G.; Levay, M.; Lindgren, R. W.; Mathur, D.; McFeaters, Edward L.; Mitchell, Sarah D.; Rehse, R.; Schrijver, Carolus J.; Springer, Larry; Stern, Robert; Tarbell, T. D.; Wüelser, Jean-Pierre; Wolfson, C. J.; Yanari, Carl; Bookbinder, Jay A.; Cheimets, Peter; Caldwell, D.; DeLuca, E. E.; Gates, Richard; Golub, L.; Park, Sang C.; Podgorski, William; Bush, R. I.; Scherrer, P. H.; Gummin, Mark A.; Smith, Peter J.; Auker, Gary; Jerram, Paul; Pool, P.; Soufli, Régina; Windt, David L.; Beardsley, S.; Clapp, Matthew; Lang, J.; Waltham, Nicholas R.

doi:10.1007/s11207-011-9776-8

Cited by 3,776 publications

(1,985 citation statements)

References 22 publications

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“…Note that the temperature responses are quite broad, and that the peak temperatures listed apply to non-flare plasmas. For details on the AIA temperature responses, see Lemen et al (2012). With AIA, coronal waves are best seen at 193 and 211Å, while the intensity enhancements become progressively weaker from 335 to 94, 131, and 304Å (see Figure 28 for an example).…”

Section: Thermal Characteristicsmentioning

confidence: 99%

“…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%

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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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Section: Thermal Characteristicsmentioning

confidence: 99%

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confidence: 99%

Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

154

140

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“…The unprecendented high spatial (plate scale of 0".6 per pixel) and temporal resolution (12 s cadence) of the SDO (Solar Dynamic Observatory) AIA experiment (Atmospheric Imaging Assembly, Lemen et al, 2012) provided novel opportunities for high quality observations of waves in plumes/interplumes regions. Krishna Prasad et al (2011Prasad et al ( , 2012 analyzed AIA data acquired at plume, interplume and in on-disk plume locations.…”

Section: Searching For Waves In 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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“…[55]. To follow larger regions in time, one can also use imaging instruments such as AIA [56] or XRT [57]. If the filtergrams span a large enough range of peak contribution temperatures, one can make a good guess at the thermal structure [58,59].…”

Section: (A) Inversions Of Observationsmentioning

confidence: 99%

What can large-scale magnetohydrodynamic numerical experiments tell us about coronal heating?

Peter

2015

Phil. Trans. R. Soc. A.

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The upper atmosphere of the Sun is governed by the complex structure of the magnetic field. This controls the heating of the coronal plasma to over a million kelvin. Numerical experiments in the form of threedimensional magnetohydrodynamic simulations are used to investigate the intimate interaction between magnetic field and plasma. These models allow one to synthesize the coronal emission just as it would be observed by real solar instrumentation. Largescale models encompassing a whole active region form evolving coronal loops with properties similar to those seen in extreme ultraviolet light from the Sun, and reproduce a number of average observed quantities. This suggests that the spatial and temporal distributions of the heating as well as the energy distribution of individual heat deposition events in the model are a good representation of the real Sun. This provides evidence that the braiding of fieldlines through magneto-convective motions in the photosphere is a good concept to heat the upper atmosphere of the Sun.

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The Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO)

Cited by 3,776 publications

References 22 publications

Large-scale Globally Propagating Coronal Waves

Large-scale Globally Propagating Coronal Waves

Solar Coronal Plumes

What can large-scale magnetohydrodynamic numerical experiments tell us about coronal heating?

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