EIT: Extreme-Ultraviolet Imaging Telescope for the Soho Mission

Delaboudiniere, J.-P.; Artzner, G. E.; Brunaud, J.; Gabriel, A. H.; Hochedez, J. F.; Millier, F.; Song, X. Y.; Au, B.; Dere, K. P.; Howard, R. A.; Kreplin, R.; Michels, D. J.; Moses, J. D.; Defise, J. M.; Jamar, C.; Rochus, P.; Chauvineau, J.P.; Marioge, J. P.; Catura, R. C.; Lemen, J. R.

doi:10.21236/ada530511

Cited by 41 publications

(48 citation statements)

References 11 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In this context, EUV imaging provides a basic measure of approaching complex active regions and the more immediate indicator of potentially Earthimpacting events such as flares and eruptions. Recent examples of such imagers include the EIT instrument [9] aboard SOHO at L1, the SDO/AIA [10], the Proba-2/SWAP instrument [11] in Earth orbit, the EUI of Solar Orbiter [12] and the EUVI instrument [13] aboard the STEREO spacecraft in solar orbit. Due to identical instrumental, observational and timing constraints at both Lagrange points, the synergies gained from a combined L1/L5 mission will be without existing comparison, allowing the perfect merge of high-resolution high-cadence EUV images for 67% of the solar surface and off solar limb.…”

Section: Biarritz France 18 -21 October 2016mentioning

confidence: 99%

Remote sensing optical instrumentation for enhanced space weather monitoring from the L1 and L5 Lagrange points

Kraft

Puschmann

Luntama

2017

International Conference on Space Optics — ICSO 2016

View full text Add to dashboard Cite

Section: Biarritz France 18 -21 October 2016mentioning

confidence: 99%

Remote sensing optical instrumentation for enhanced space weather monitoring from the L1 and L5 Lagrange points

Kraft

Puschmann

Luntama

2017

International Conference on Space Optics — ICSO 2016

View full text Add to dashboard Cite

“…The EUV/EIT data (Delaboudinière et al, 1995) selected from the SOHO archive correspond to i) level zero data, with ii) science objective as "FULL SUN 171/284/195/304," and iii) object as "full FOV." The data thus consist of four synoptic fulldisk and full-resolution images taken, in general, every six hours at the four wavelengths, one at the chromosphere/transition region interface (He II 304 Å) and three corresponding to coronal temperatures (Fe IX/X 171, Fe XII 195, and Fe XV 284 Å).…”

Section: Overview Of Approach and Data Selectionmentioning

confidence: 99%

Automatic Detection and Classification of Coronal Holes and Filaments Based on EUV and Magnetogram Observations of the Solar Disk

Scholl

Habbal

2007

Sol Phys

View full text Add to dashboard Cite

A new method for the automated detection of coronal holes and filaments on the solar disk is presented. The starting point is coronal images taken by the Extreme Ultraviolet Telescope on the Solar and Heliospheric Observatory (SOHO/EIT) in the Fe IX/X 171 Å, Fe XII 195 Å, and He II 304 Å extreme ultraviolet (EUV) lines and the corresponding full-disk magnetograms from the Michelson Doppler Imager (SOHO/MDI) from different phases of the solar cycle. The images are processed to enhance their contrast and to enable the automatic detection of the two candidate features, which are visually indistinguishable in these images. Comparisons are made with existing databases, such as the He I 10830 Å NSO/Kitt Peak coronal-hole maps and the Solar Feature Catalog (SFC) from the European Grid of Solar Observations (EGSO), to discriminate between the two features. By mapping the features onto the corresponding magnetograms, distinct magnetic signatures are then derived. Coronal holes are found to have a skewed distribution of magnetic-field intensities, with values often reaching 100 -200 gauss, and a relative magnetic-flux imbalance. Filaments, in contrast, have a symmetric distribution of field intensity values around zero, have smaller magnetic-field intensity than coronal holes, and lie along a magnetic-field reversal line. The identification of candidate features from the processed images and the determination of their distinct magnetic signatures are then combined to achieve the automated detection of coronal holes and filaments from EUV images of the solar disk. Application of this technique to all three wavelengths does not yield identical results. Furthermore, the best agreement among all three wavelengths and NSO/Kitt Peak coronal-hole maps occurs during the declining phase of solar activity. The He II data mostly fail to yield the location of filaments at solar 426 I.F. Scholl, S.R. Habbal minimum and provide only a subset at the declining phase or peak of the solar cycle. However, the Fe IX/X 171 Å and Fe XII 195 Å data yield a larger number of filaments than the Hα data of the SFC.

show abstract

“…The eruptive filament bifurcated and transformed into a large Y-shaped cloud, which moved from the region of bifurcation (Rb) to the South-West across the solar disk toward the limb. Figure 1 illustrates what has happened to the eruptive filament, as shown by the Hα images produced by the Kanzelhöhe Solar Observatory (KSO), the Extreme-ultraviolet Imaging Telescope (EIT; Delaboudinière et al, 1995), on board the Solar and Heliospheric Observatory (SOHO), and the Spectroheliographic X-ray Imaging Telescope (SPIRIT; Zhitnik et al (2002) and Slemzin et al (2005)), on board the Complex Orbital near-Earth Observations of Activity of the Sun (CORONAS-F) satellite (Oraevsky and Sobelman, 2002;Oraevsky et al, 2003).…”

Section: Introductionmentioning

confidence: 99%

A Challenging Solar Eruptive Event of 18 November 2003 and the Causes of the 20 November Geomagnetic Superstorm. III. Catastrophe of the Eruptive Filament at a Magnetic Null Point and Formation of an Opposite-Handedness CME

et al. 2014

View full text Add to dashboard Cite

Our analysis in Papers I and II (Grechnev et al., 2014, Solar Phys. 289, 289 and 1279) of the 18 November 2003 solar event responsible for the 20 November geomagnetic superstorm has revealed a complex chain of eruptions. In particular, the eruptive filament encountered a topological discontinuity located near the solar disk center at a height of about 100 Mm, bifurcated, and transformed into a large cloud, which did not leave the Sun. Concurrently, an additional CME presumably erupted close to the bifurcation region. The conjectures about the responsibility of this compact CME for the superstorm and its disconnection from the Sun are confirmed in Paper IV (Grechnev et al., Solar Phys., submitted), which concludes about its probable spheromak-like structure. The present paper confirms the presence of a magnetic null point near the bifurcation region and addresses the origin of the magnetic helicity of the interplanetary magnetic clouds and their connection to the Sun. We find that the orientation of a magnetic dipole constituted by dimmed regions with the opposite magnetic polarities away from the parent active region corresponded to the direction of the axial field in the magnetic cloud, while the pre-eruptive filament mismatched it. To combine all of the listed findings, we come to an intrinsically three-dimensional scheme, in which a spheromak-like eruption originates via the interaction of the initially unconnected magnetic fluxes of the eruptive filament and pre-existing ones in the corona. Through a chain of magnetic reconnections their positive mutual helicity was transformed into the self-helicity of the spheromak-like magnetic cloud.

show abstract

EIT: Extreme-Ultraviolet Imaging Telescope for the Soho Mission

Cited by 41 publications

References 11 publications

Remote sensing optical instrumentation for enhanced space weather monitoring from the L1 and L5 Lagrange points

Remote sensing optical instrumentation for enhanced space weather monitoring from the L1 and L5 Lagrange points

Automatic Detection and Classification of Coronal Holes and Filaments Based on EUV and Magnetogram Observations of the Solar Disk

A Challenging Solar Eruptive Event of 18 November 2003 and the Causes of the 20 November Geomagnetic Superstorm. III. Catastrophe of the Eruptive Filament at a Magnetic Null Point and Formation of an Opposite-Handedness CME

Contact Info

Product

Resources

About