The EUV Imaging Spectrometer for Hinode

Culhane, J. L.; Harra, L. K.; James, Ady; Al-Janabi, K.; Bradley, L.; Chaudry, R. A.; Rees, K.; Tandy, J. A.; Thomas, Padmaja B.; Whillock, M. C. R.; Winter, B.; Doschek, G. A.; Korendyke, C. M.; Brown, C. M.; Myers, S. H.; Mariska, J. T.; Seely, John F.; Lang, J.; Kent, B. J.; Shaughnessy, Bryan; Young, Peter R.; Simnett, G. M.; Castelli, C.; Mahmoud, Saad; Mapson-Menard, H.; Probyn, B. J.; Thomas, R. J.; Davila, J. M.; Dere, K. P.; Windt, David L.; Shea, J.; Hagood, R.; Moye, Robert W.; Hara, Hirohisa; Watanabe, Tetsuya; Matsuzaki, Keiichi; Kosugi, T.; Hansteen, V. H.; Wikstøl, Ø.

doi:10.1007/978-0-387-88739-5_7

Cited by 19 publications

(23 citation statements)

References 35 publications

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“…Mixed polarity areas were associated with smaller blueshifts. Tian et al (2010) examined HINODE/EIS EUV Imaging Spectrometer (Culhane et al, 2007) data, focussing on the Ne viii behavior and complementary SUMER observations, confirming the occurrence of larger blueshifts The chromospheric magnetic network boundaries inferred from Si ii images has been superposed to the Ne viii (temperature of formation log = 5.8) map, to facilitate the identification of the origin of the highest blueshifts. The zero velocity reference has been identified by using off-limb unbinned data and a moment technique to fit the line profiles.…”

Section: Plume Outflows In the Low Coronamentioning

confidence: 89%

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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Section: Plume Outflows In the Low Coronamentioning

confidence: 89%

Solar Coronal Plumes

Poletto

2015

Living Rev. Sol. Phys.

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“…Spectroscopic measurements are made using the EUV Imaging Spectrometer (EIS; Culhane et al, 2007) onboard Hinode. The data we use are 1 slit coarse (2 ) raster scans of a 120 × 512 field-of-view, taking 60-second exposures at each position.…”

Section: Data Sources and Processingmentioning

confidence: 99%

On-Disc Observations of Flux Rope Formation Prior to Its Eruption

et al. 2017

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Coronal mass ejections (CMEs) are one of the primary manifestations of solar activity and can drive severe space weather effects. Therefore, it is vital to work towards being able to predict their occurrence. However, many aspects of CME formation and eruption remain unclear, including whether magnetic flux ropes are present before the onset of eruption and the key mechanisms that cause CMEs to occur. In this work, the pre-eruptive coronal configuration of an active region that produced an interplanetary CME with a clear magnetic flux rope structure at 1 AU is studied. A forward-S sigmoid appears in extremeultraviolet (EUV) data two hours before the onset of the eruption (SOL2012-06-14), which is interpreted as a signature of a right-handed flux rope that formed prior to the eruption. Flare ribbons and EUV dimmings are used to infer the locations of the flux rope footpoints. These locations, together with observations of the global magnetic flux distribution, indicate that an interaction between newly emerged magnetic flux and pre-existing sunspot field in the days prior to the eruption may have enabled the coronal flux rope to form via tethercutting-like reconnection. Composition analysis suggests that the flux rope had a coronal plasma composition, supporting our interpretation that the flux rope formed via magnetic reconnection in the corona. Once formed, the flux rope remained stable for two hours before erupting as a CME. Electronic supplementary material The online version of this article

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“…Several EUV spectrometers have helped in characterizing the physical parameters of coronal waves and associated phenomena: CDS (Harrison et al, 1995) and UVCS (Kohl et al, 1995) aboard SOHO, and EIS (Culhane et al, 2007) aboard Hinode. In the radio regime, the bulk of the information about wave-associated metric type II bursts comes from various ground-based radiospectrographs and radioheliographs.…”

Section: Observational Signaturesmentioning

confidence: 99%

Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

164

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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The EUV Imaging Spectrometer for Hinode

Cited by 19 publications

References 35 publications

Solar Coronal Plumes

Solar Coronal Plumes

On-Disc Observations of Flux Rope Formation Prior to Its Eruption

Large-scale Globally Propagating Coronal Waves

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