EIT: Extreme-UltraViolet Imaging Telescope for the SOHO Mission

Delaboudinière, J. P.; Artzner, G.; Brunaud, J.; Gabriel, A. H.; Hochedez, Jean-François; Millier, F.; Song, Xueyan; Au, B.; Dere, K. P.; Howard, R. A.; Kreplin, R. W.; Michels, D. J.; Moses, J. D.; Defise, Jean-Marc; Jamar, C.; Rochus, Pierre; Chauvineau, J.P.; Marioge, J P; Catura, R. C.; Lemen, J. R.; Shing, L.; Stern, Robert; Gurman, J. B.; Neupert, W. M.; Maucherat, A.; Clette, F.; Cugnon, P.; Dessel, E. L. van

doi:10.1007/978-94-009-0191-9_8

Cited by 157 publications

(164 citation statements)

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“…In its standard operating mode, the AIA images the entire Sun ten times faster per wavelength than TRACE at twice the number of coronal channels, with a 16-fold increase in the number of pixels per image. Compared with the full-disk SOHO/EIT (Delaboudinière et al, 1995), AIA runs at 700× the usual EIT image frequency, with 16 times more pixels per image, in typically eight instead of four channels. Compared to EIT and TRACE, the AIA thus represents an increase in the information rate for coronal observations by a factor of 400 to 22 000.…”

Section: Figurementioning

confidence: 99%

The Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO)

et al. 2011

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Section: Figurementioning

confidence: 99%

The Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO)

et al. 2011

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“…CDS observations in the helium lines He I 58.4 nm, 53.7 nm and He II at 30.4 nm (and other EUV lines) in combination with synoptic observations by the Extreme-ultraviolet Imaging Telescope (EIT; Delaboudinière et al 1995) led Andretta et al (2003) to the conclusion that the photoionization-recombination mechanism alone cannot explain the formation of He II 30.4 nm. Andretta and Jones (1997), on theoretical grounds, favour a two-layer formation model of the helium spectrum with mixed contributions of the excitation processes.…”

Section: The Helium Emissionsmentioning

confidence: 99%

Observations of the Sun at Vacuum-Ultraviolet Wavelengths from Space. Part II: Results and Interpretations

et al. 2007

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In Part I of this review, the concepts of solar vacuum-ultraviolet (VUV) observations were outlined together with a discussion of the space instrumentation used for the investigations. A section on spectroradiometry provided some quantitative results on the solar VUV radiation without considering any details of the solar phenomena leading to the radiation. Here, in Part II, we present solar VUV observations over the last decades and their interpretations in terms of the plasma processes and the parameters of the solar atmosphere, with emphasis on the spatial and thermal structures of the chromosphere, transition region and corona of the quiet Sun. In addition, observations of active regions, solar flares and prominences are included as well as of small-scale events. Special sections are devoted to the elemental composition of the solar atmosphere and theoretical considerations on the heating of the corona and the generation of the solar wind.

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“…On 27-29 May 2003 the EUV Imaging Telescope (EIT, Delaboudinière et al, 1995) on board SOHO was in "CME watch" mode (12-min cadence), in the 30.4-nm line of He II (formed in the chromosphere to corona transition region at 0.8 MK). This mode allows the observation of the initial phase of CMEs.…”

Section: The Solar Active Region Ar 10365mentioning

confidence: 99%

From the Sun to the Earth: impact of the 27-28 May 2003 solar events on the magnetosphere, ionosphere and thermosphere

et al. 2006

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Abstract. During the last week of May 2003, the solar active region AR 10365 produced a large number of flares, several of which were accompanied by Coronal Mass Ejections (CME). Specifically on 27 and 28 May three halo CMEs were observed which had a significant impact on geospace. On 29 May, upon their arrival at the L1 point, in front of the Earth's magnetosphere, two interplanetary shocks and two additional solar wind pressure pulses were recorded by the ACE spacecraft. The interplanetary magnetic field data showed the clear signature of a magnetic cloud passing ACE. In the wake of the successive increases in solar wind pressure, the magnetosphere became strongly compressed and the sub-solar magnetopause moved inside five Earth radii. At low altitudes the increased energy input to the magnetosphere was responsible for a substantial enhancement of Region-1 field-aligned currents. The ionospheric Hall currents also intensified and the entire high-latitude current system moved equatorward by about 10 • . Several substorms occurred during this period, some of them -but not allapparently triggered by the solar wind pressure pulses. The storm's most notable consequences on geospace, including space weather effects, were (1) the expansion of the auroral oval, and aurorae seen at mid latitudes, (2) the significant modification of the total electron content in the sunlight highlatitude ionosphere, (3) the perturbation of radio-wave propagation manifested by HF blackouts and increased GPS signal scintillation, and (4) the heating of the thermosphere, causing

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EIT: Extreme-UltraViolet Imaging Telescope for the SOHO Mission

Cited by 157 publications

References 12 publications

The Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO)

The Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO)

Observations of the Sun at Vacuum-Ultraviolet Wavelengths from Space. Part II: Results and Interpretations

From the Sun to the Earth: impact of the 27-28 May 2003 solar events on the magnetosphere, ionosphere and thermosphere

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