Prominence Cavity Regions Observed Using SWAP 174 Å Filtergrams and Simultaneous Eclipse Flash Spectra

Bazin, C.; Koutchmy, S.; Tavabi, E.

doi:10.1007/s11207-012-0188-1

Cited by 6 publications

(5 citation statements)

References 23 publications

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“…Mk4; see Byrne et al, 2014), or complementary eclipse observations (e.g. Pasachoff et al, 2011Pasachoff et al, , 2015Bazin, Koutchmy, and Tavabi, 2013), although these observations are intermittent and cannot be used on a continuous basis. The observational gap is gradually being filled with new EUV and WL instruments.…”

Section: Discussionmentioning

confidence: 99%

“…Cavities are believed to be the density-depleted cross sections of the magnetic-flux ropes, where the magnetic-field strength has attained greater values than the background corona (Rachmeler et al, 2013). Bazin, Koutchmy, and Tavabi (2013) compared off-limb SWAP observations of a couple of prominence and cavity structures to simultaneous, slitless flash spectra obtained during the total solar eclipse of 11 July 2010. The flash spectra (see description by Bazin, Koutchmy, and Tavabi, 2013) were used to measure the continuum emission outside the prominences, and to study the electron density of the cavity.…”

Section: Prominences and Cavitiesmentioning

confidence: 99%

“…Bazin, Koutchmy, and Tavabi (2013) compared off-limb SWAP observations of a couple of prominence and cavity structures to simultaneous, slitless flash spectra obtained during the total solar eclipse of 11 July 2010. The flash spectra (see description by Bazin, Koutchmy, and Tavabi, 2013) were used to measure the continuum emission outside the prominences, and to study the electron density of the cavity. Intensity deficits were observed and measured at the boundaries of cavities in both eclipse and SWAP images.…”

Section: Prominences and Cavitiesmentioning

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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Section: Discussionmentioning

confidence: 99%

Section: Prominences and Cavitiesmentioning

confidence: 99%

Section: Prominences and Cavitiesmentioning

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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“…SWAP observations have been used to study large-scale coronal structures such as streamers/pseudostreamers (Rachmeler et al., 2014 ; Goryaev et al., 2014 ; Guennou et al., 2016 ), prominence cavity regions (Bazin, Koutchmy, and Tavabi, 2013 ), post-flare giant arches (West and Seaton, 2015 ), and coronal mass ejections (O’Hara et al., 2019 ). Observations of such large-scale structures, in particular persistent structures such as streamers/pseudostreamers and coronal fans (Koutchmy and Nikoghossian, 2002 ; Morgan and Habbal, 2007 ), can help validate and inform the development of global coronal magnetic field models.…”

Section: Introductionmentioning

confidence: 99%

Investigation of the Middle Corona with SWAP and a Data-Driven Non-Potential Coronal Magnetic Field Model

et al. 2020

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The large field-of-view of the Sun Watcher using Active Pixel System detector and Image Processing (SWAP) instrument onboard the PRoject for Onboard Autonomy 2 (PROBA2) spacecraft provides a unique opportunity to study extended coronal structures observed in the EUV in conjunction with global coronal magnetic field simulations. A global non-potential magnetic field model is used to simulate the evolution of the global corona from 1 September 2014 to 31 March 2015, driven by newly emerging bipolar active regions determined from Helioseismic and Magnetic Imager (HMI) magnetograms. We compare the large-scale structure of the simulated magnetic field with structures seen off-limb in SWAP EUV observations. In particular, we investigate how successful the model is in reproducing regions of closed and open structures, the scale of structures, and compare the evolution of a coronal fan observed over several rotations. The model is found to accurately reproduce observed large-scale, off-limb structures. When discrepancies do arise they mainly occur off

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“…Eclipse slitless flash spectra were obtained during the second contact, just before the totality of the solar eclipse of 11 July 2010 observed in French Polynesia. We used the grating objective technique and fast CCD imaging (see Bazin, Koutchmy and Tavabi 2012). The motivations are to try to explain some similarities between the high First Ionisation Potential-FIP of helium lines intensity ratio in the Chromosphere-Corona Interface CCI and the Prominence to Corona Interface PCI.…”

Section: Introductionmentioning

confidence: 99%

Observation of the prominence cavity region using slitless eclipse flash spectra and space borne EUV filtergrams

Bazin¹,

Koutchmy²,

Lamy³

et al. 2013

Proc. IAU

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We used total solar eclipse free of parasitic light for studying the prominence to corona interface, and the corresponding cavity in the context of the coronal physics. We analysed the visible continuum between the prominences to directly look at the electron density. We demonstrate some enhanced heating in the cavity region. Some similarities with the interface regions are shown: the photosphere to the chromosphere and the prominence to the corona interface. The optically thin neutral Helium at 4713 Å and the singly ionized Helium 4686 Å Paschen α lines are considered. We summed 80 slitless visible eclipse flash spectra that we compare with simultaneously obtained EUV SWAP/Proba2 174 Å images of ESA and AIA/SDO 171Å 193 Å 304 Å and 131 Å filtergrams. Intensity profiles in a radial direction are studied. We deduce the variation of the intensity ratio I(He I 4713) / I(He II 4686). Discussion: the temperature rises at the edge of the prominences. We evaluate for the first time with spectrophotometric accuracy the continuum modulations in prominence spectra. W-L intensity deficits are observed near the prominence boundaries in both eclipse spectra and in EUV images, confirming that the prominence -cavity regions correspond to a relative depression of plasma density of the surrounding corona. Conclusion: we demonstrate some enhanced heating occurring in these regions assuming hydrostatic equilibrium.

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Prominence Cavity Regions Observed Using SWAP 174 Å Filtergrams and Simultaneous Eclipse Flash Spectra

Cited by 6 publications

References 23 publications

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

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

Investigation of the Middle Corona with SWAP and a Data-Driven Non-Potential Coronal Magnetic Field Model

Observation of the prominence cavity region using slitless eclipse flash spectra and space borne EUV filtergrams

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