The GOES‐R Solar UltraViolet Imager

Darnel, Jonathan; Seaton, Daniel B.; Rachmeler, Laurel; Jarvis, Alison; Hill, S. M.; Peck, Courtney; Hughes, J. Marcus; Shapiro, Jason; Riley, Allyssa; Vasudevan, Gopal; Shing, L.; Koener, George; Edwards, Christopher G.; Mathur, D.; Timothy, Shelbe

doi:10.1029/2022sw003044

Cited by 19 publications

(19 citation statements)

References 48 publications

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“…We used images from a special off-pointing campaign of the Geostationary Operational Environmental Satellite's (GOES) Solar Ultraviolet Imager (SUVI) 20,21 that directly observed the middle corona to identify coronal dynamics associated with the highly structured slow solar wind. The extended field of view of SUVI allowed us to trace extreme-ultraviolet (EUV) features up to a height of about 2.7 R ☉ , into the middle corona (Methods).…”

Section: Resultsmentioning

confidence: 99%

Direct observations of a complex coronal web driving highly structured slow solar wind

et al. 2022

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The solar wind consists of continuous streams of charged particles that escape into the heliosphere from the Sun, and is split into fast and slow components, with the fast wind emerging from the interiors of coronal holes. Near the ecliptic plane, the fast wind from low-latitude coronal holes is interspersed with a highly structured slow solar wind, the source regions and drivers of which are poorly understood. Here we report extreme-ultraviolet observations that reveal a spatially complex web of magnetized plasma structures that persistently interact and reconnect in the middle corona. Coronagraphic white-light images show concurrent emergence of slow wind streams over these coronal web structures. With advanced global magnetohydrodynamics coronal models, we demonstrate that the observed coronal web is a direct imprint of the magnetic separatrix web (S-web). By revealing a highly dynamic portion of the S-web, our observations open a window into important middle-coronal processes that appear to play a key role in driving the structured slow solar wind.

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Section: Resultsmentioning

confidence: 99%

Direct observations of a complex coronal web driving highly structured slow solar wind

et al. 2022

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“…Other EUV telescopes that observed the eruption were: the EUVI (Howard et al 2008) aboard the STEREO A spacecraft, with a cadence of ∼3 min; the AIA (Lemen et al 2012) aboard the Solar Dynamics Observatory (SDO; Pesnell et al 2012), with a cadence of 12 s; the SUVI (Darnel et al 2022) aboard Geostationary Operational Environmental Satellite-16 (GOES-16), with a cadence of ∼4 min; and the Sun Watcher using Active Pixel (SWAP; Seaton et al 2013) sensor aboard the PRoject for On Board Autonomy 2 (PROBA2; Santandrea et al 2013) space-craft, with a cadence of ∼2 min. The corresponding CME was subsequently observed in white light by the COR1 and COR2 coronagraphs (Howard et al 2008) aboard STEREO A, with cadences of 5 min and 15 min, respectively, and by LASCO (Brueckner et al 1995) aboard SOHO (Domingo et al 1995), with a 12-minute cadence.…”

Section: Summary and Discussionmentioning

confidence: 99%

Prominence eruption observed in He II 304 Å up to >6 R_⊙ by EUI/FSI aboard Solar Orbiter

Mierla

Zhukov

Berghmans

et al. 2022

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Aims. We report observations of a unique, large prominence eruption that was observed in the He II 304 Å passband of the the Extreme Ultraviolet Imager/Full Sun Imager telescope aboard Solar Orbiter on 15-16 February 2022. Methods. Observations from several vantage points -Solar Orbiter, the Solar-Terrestrial Relations Observatory, the Solar and Heliospheric Observatory, and Earth-orbiting satellites -were used to measure the kinematics of the erupting prominence and the associated coronal mass ejection. Three-dimensional reconstruction was used to calculate the deprojected positions and speeds of different parts of the prominence. Observations in several passbands allowed us to analyse the radiative properties of the erupting prominence.Results. The leading parts of the erupting prominence and the leading edge of the corresponding coronal mass ejection propagate at speeds of around 1700 km s −1 and 2200 km s −1 , respectively, while the trailing parts of the prominence are significantly slower (around 500 km s −1 ). Parts of the prominence are tracked up to heights of over 6 R . The He II emission is probably produced via collisional excitation rather than scattering. Surprisingly, the brightness of a trailing feature increases with height. Conclusions. The reported prominence is the first observed in He II 304 Å emission at such a great height (above 6 R ).

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“…Blooming can lead to loss of information not just in the saturated pixel but also in surrounding pixels. The SUVI instrument, the large-FOV imager on the GOES-R platforms, has incorporated antiblooming circuitry in its CCD to avoid blooming-saturated pixels (Darnel et al, 2022), allowing SUVI to observe extremely bright features, such as solar flares, without the destructive image effects of blooming.…”

Section: Discussionmentioning

confidence: 99%

“…SUVI has been making periodic off-point observations of the extended EUV atmosphere since 2019 (Darnel et al, 2022). Seaton et al (2021) used SUVI to carry out the first comprehensive study of the dynamics of the extended EUV atmosphere through multiple bandpasses on long timescales.…”

Section: Discussionmentioning

confidence: 99%

“…4, 13.1, 17.1, 19.3, 21.1, 30.4, and 33.5 nm. Since 2017 the Solar Ultraviolet Imager (SUVI: Darnel et al, 2022), on the several Geostationary Operational Environmental Satellite (GOES-R) spacecraft, has been observing through six passbands, with peak wavelengths at 9. 4, 13.1, 17.1, 19.5, 28.4, and 30.4 nm, through a similar FOV to SWAP of ≈ 53 .…”

Section: Swap Observationsmentioning

confidence: 99%

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A Review of the Extended EUV Corona Observed by the Sun Watcher with Active Pixels and Image Processing (SWAP) Instrument

et al. 2022

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The Sun Watcher with Active Pixels and Image Processing (SWAP) instrument onboard ESA’s PRoject for On Board Autonomy 2 (PROBA2) has provided the first uncompressed, high-cadence, continuous, large field-of-view observations of the extended extreme-ultraviolet (EUV) corona for over a complete solar cycle. It has helped shape our understanding of this previously understudied region, and pioneered research into the middle corona. In this article, we present a review of all publications that have utilized these observations to explore the extended EUV corona, highlighting the unique contributions made by SWAP. The review is broadly divided into three main sections of SWAP-based studies about: i) long-lived phenomena, such as streamers, pseudo-streamers, and coronal fans; ii) dynamic phenomena, such as eruptions, jets, EUV waves, and shocks; iii) coronal EUV emission generation. We also highlight SWAP’s imaging capabilities, techniques that have been applied to observations to enhance the off-limb observations and its legacy.

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The GOES‐R Solar UltraViolet Imager

Cited by 19 publications

References 48 publications

Direct observations of a complex coronal web driving highly structured slow solar wind

Direct observations of a complex coronal web driving highly structured slow solar wind

Prominence eruption observed in He II 304 Å up to >6 R_⊙ by EUI/FSI aboard Solar Orbiter

A Review of the Extended EUV Corona Observed by the Sun Watcher with Active Pixels and Image Processing (SWAP) Instrument

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The GOES‐R Solar UltraViolet Imager

Cited by 19 publications

References 48 publications

Direct observations of a complex coronal web driving highly structured slow solar wind

Direct observations of a complex coronal web driving highly structured slow solar wind

Prominence eruption observed in He II 304 Å up to >6 R⊙ by EUI/FSI aboard Solar Orbiter

A Review of the Extended EUV Corona Observed by the Sun Watcher with Active Pixels and Image Processing (SWAP) Instrument

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Prominence eruption observed in He II 304 Å up to >6 R_⊙ by EUI/FSI aboard Solar Orbiter