Structure and Dynamics of the 2010 July 11 Eclipse White-Light Corona

Pasachoff, Jay M.; Rusin, V.; Druckmüllerová, Hana; Санига, Метод; Lu, M.; Malamut, C.; Seaton, Daniel B.; Golub, L.; Engell, Alexander; Hill, Steven; Lucas, R.

doi:10.1088/0004-637x/734/2/114

Cited by 27 publications

(22 citation statements)

References 29 publications

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“…The deficiency values at 195A are surprisingly found to be only about 6.6 %, without taking into account the effect of the spurious scattered light (stray light effect). In this "hotter" emission line of about 1.5 MK the cavity contrast seems reduced, a result similar to the one recently described by Habbal et al (2010 and2011) and by Pasachoff et al (2011) for eclipse cavities. Moreover in Fig.…”

Section: ) Photometric Analysis Of the Cavity Regions In W-l With Ssupporting

confidence: 89%

“…The total eclipse of 11 th July 2010 (Pasachoff et al 2011and Habbal et al 2010-2011 for a description of the corona at this eclipse), allowed us to observe the true continuum between helium prominence lines (He I 4713A and Pα He II 4686A), taking into account faint low excitation emission lines using fast slitless spectra taken at the contacts, before and after the totality. These observations also yield relatively new results on the determination of the electron densities inside prominences when compared to previous photographic ground-based coronagraphic filtergram observations in the D3 line, where the continuum, at the location of the prominences, was not precisely measured (see Kubota and Leroy, 1970 for Lyotcoronagraph observations and Koutchmy, Lebecq and Stellmacher 1983 for eclipse broadband observations).…”

Section: I) Introductionmentioning

confidence: 99%

“…Here we have the advantage of having many W-L images of the corona taken during the eclipse totality (Pasachoff et al 2011, Habbal et al 2011.…”

Section: I) Introductionmentioning

confidence: 99%

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

2012

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Abstract:Images from the SWAP (Proba 2 mission) taken at 174A in the Fe IX/X lines are compared to simultaneous slitless flash spectra taken during the last solar total eclipse of July, 11 th 2010. Many faint low excitation emission lines together with the HeI and HeII Paschen Alpha chromospheric lines are recorded on eclipse spectra where regions of limb prominences are obtained with space-borne imagers. We consider a deep flash spectrum obtained by summing 80 individual spectra to show the intensity modulations of the continuum. Intensity depressions are observed around the prominences in both eclipse and SWAP images. The prominence cavities are interpreted as a relative depression of plasma density, produced inside the corona surrounding the prominences. Photometric measurements are shown at different scales and different, spectrally narrow, intervals for both the prominences and the coronal background.

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Section: ) Photometric Analysis Of the Cavity Regions In W-l With Ssupporting

confidence: 89%

Section: I) Introductionmentioning

confidence: 99%

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

2012

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“…A comparison of the observations from the two sites separated by 93 minutes appeared in Pasachoff et al (2011). The thermodynamics of the corona and the observed evolution of the magnetic field during this same eclipse was described in Habbal et al (2011).…”

Section: Wg On Solar Eclipses (Jay M Pasachoff )mentioning

confidence: 63%

DIVISION II: SUN and HELIOSPHERE

Pillet¹,

Klimchuk²,

Melrose³

et al. 2011

Proc. IAU

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“…Such observation campaigns have been useful in filling in gaps between the low corona, which is visible in EUV or white-light eclipse images, and more extended features that are seen in coronagraph images from instruments such as LASCO (e.g. Pasachoff et al, 2011 andSlemzin et al, 2012). Software for combining several off-pointed images into single mosaic images is provided in SWAP's SolarSoft library.…”

Section: Commanded Spacecraft Operationsmentioning

confidence: 99%

The SWAP EUV Imaging Telescope Part I: Instrument Overview and Pre-Flight Testing

et al. 2012

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The Sun Watcher with Active Pixels and Image Processing (SWAP) is an EUV solar telescope on board ESA's Project for Onboard Autonomy 2 (PROBA2) mission launched on 2 November 2009. SWAP has a spectral bandpass centered on 17.4 nm and provides images of the low solar corona over a 54×54 arcmin field-of-view with 3.2 arcsec pixels and an imaging cadence of about two minutes. SWAP is designed to monitor all space-weather-relevant events and features in the low solar corona. Given the limited resources of the PROBA2 microsatellite, the SWAP telescope is designed with various innovative technologies, including an off-axis optical design and a CMOS-APS detector. This article provides reference documentation for users of the SWAP image data.

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Structure and Dynamics of the 2010 July 11 Eclipse White-Light Corona

Cited by 27 publications

References 29 publications

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

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

DIVISION II: SUN and HELIOSPHERE

The SWAP EUV Imaging Telescope Part I: Instrument Overview and Pre-Flight Testing

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