The Coronal Diagnostic Spectrometer for the solar and heliospheric observatory

Harrison, R. A.; Sawyer, Eric; Carter, M. K.; Cruise, A. M.; Cutler, R. M.; Fludra, A.; Hayes, R. W.; Kent, B. J.; Lang, J.; Parker, David; Payne, J.; Pike, C. D.; Peskett, S. C.; Richards, A. G.; Gulhane, J. L.; Norman, K.; Breeveld, A. A.; Breeveld, E. R.; Janabi, K. F. Al; McCalden, A. J.; Parkinson, J. H.; Self, D.; Thomas, Padmaja B.; Poland, A. I.; Thomas, R. J.; Thompson, W. T.; Kjeldseth-Moe, O.; Brekke, P.; Karud, J.; Maltby, P.; Aschenbach, B.; Bräuninger, H.; Kühne, M.; Hollandt, J.; Siegmund, O. H. W.; Huber, M. C. E.; Gabriel, A. H.; Mason, H. E.; Bromage, B. J. I.

doi:10.1007/bf00733431

Cited by 481 publications

(132 citation statements)

References 29 publications

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“…emitted intensity) observations at solar-disk center. The comparisons use some quiet-Sun atlases derived from the following instruments: Solar Ultraviolet Measurements of Emitted Radiation (SUMER: Wilhelm et al, 1995) onboard SOHO, EUV Imaging Spectrometer (EIS: Culhane et al, 2007) onboard Hinode, and the Coronal Diagnostic Spectrometer (CDS: Harrison et al, 1995) onboard SOHO. In all cases, we convolved the computed spectrum with the instrument resolution, which is known for the first two instruments but lesser understood for CDS.…”

Section: Comparison Of Emitted Intensity (Radiance) With Observationsmentioning

confidence: 99%

Far- and Extreme-UV Solar Spectral Irradiance and Radiance from Simplified Atmospheric Physical Models

et al. 2013

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This article describes an update of the physical models that we use to reconstruct the FUV and EUV irradiance spectra and the radiance spectra of the features that at any given point in time may cover the solar disk depending on the state of solar activity. The present update introduces important modifications to the chromosphere-corona transition region of all models. Also, the update introduces improved and extended atomic data. By these changes, the agreement of the computed and observed spectra is largely improved in many EUV lines important for the modeling of the Earth's upper atmosphere. This article describes the improvements and shows detailed comparisons with EUV/FUV radiance and irradiance measurements. The solar spectral irradiance from these models at wavelengths longer than ≈ 200 nm is discussed in a separate article.

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Section: Comparison Of Emitted Intensity (Radiance) With Observationsmentioning

confidence: 99%

Far- and Extreme-UV Solar Spectral Irradiance and Radiance from Simplified Atmospheric Physical Models

et al. 2013

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“…CDS (Harrison et al 1995) observed the prominences within a large 240 × 240 raster in 6 lines (duration 50 min) followed by 120 × 240 rasters in 14 lines (duration 30 min). The prominences are seen in emission in the transition-region lines and as dark regions in coronal lines.…”

Section: Cdsmentioning

confidence: 99%

SOHO/SUMER observations and analysis of the hydrogen Lyman spectrum in solar prominences

Heinzel

Schmieder

Vial

et al. 2001

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Abstract. The complete hydrogen Lyman spectrum in several prominences has been observed with the UV spectrometer SUMER on-board the SOHO, during the Joint Observing Programme 107, together with other space and ground-based observatories. Based on these observations, we are able to demonstrate, for the first time, that there exists a large variety of intensities and shapes of Lyman lines in different prominences and in various parts thereof. Therefore, no "canonical" Lyman spectrum can be considered for modelling purposes. However, we have identified at least two representative properties of the observed spectra: in one case (May 28, 1999 prominence) we detected high integrated intensities and no reversals in lines higher than Lα. Another prominence (June 2, 1999) exhibited quite similar integrated intensities, but all lines have rather strongly reversed profiles. This behaviour cannot be explained in terms of standard isothermal-isobaric models and we thus consider more general models which are in pressure equilibrium with the magnetic field and which have significant prominencecorona transition region (PCTR) temperature gradients. This type of model, recently suggested by Anzer & Heinzel (1999), is capable of explaining strong emission profiles without reversal. Based on extended non-LTE computations, we suggest that quite different Lyman spectra mentioned above may correspond to two types of PCTRs, one seen along the magnetic-field lines (unreversed profiles) and the other one seen across the field lines (reversed profiles). Finally, we again confirm the importance of partial-redistribution (PRD) scattering processes for Lyman lines in prominences. However, our analysis of new SUMER data also points to a critical role of the PCTR in radiative transport in these lines.

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“…Vrsnak et al (1990) report damped post-eruptive oscillations in an active prominence, but clear observations of prominences at limb during their eruption are extremely rare (Berger et al 2010). We focus here on the analysis of two active filaments, observed during their eruption, from two sets of observations performed at high cadence: one with the Coronal Diagnostic Spectrometer (CDS) (Harrison et al 1995) on-board SOHO (Fleck et al 1995) and one with the NSO/Dunn Solar Telescope (DST). These data sets are complemented by observations from the extreme UV imager EIT on-board SOHO and the soft X-ray telescope (SXT) onboard Yohkoh.…”

Section: Introductionmentioning

confidence: 99%

Oscillatory motions observed in eruptive filaments

Bocchialini

Baudin

Koutchmy

et al. 2011

A&A

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Context. The origin of the variable component of the solar wind is of great intrinsic interest for heliophysics and spaceweather, e.g. the initiation of coronal mass ejections and the problem of mass loss of all stars. It is also related to the physics of coronal neutral sheets and streamers, which occur above lines of magnetic polarity reversal. Filaments and prominences correspond to the cool coronal component of these regions. Aims. We examine the dynamical behaviour of these structures where reconnection and dissipation of magnetic energy in the turbulent plasma are occurring. The link between the observed oscillatory motions and the eruption occurrence is investigated in detail for two different events. Methods. Two filaments were analysed using two different datasets: time series of spectra using a transition region line (He I at 584.33 Å) and a coronal line (Mg X at 609.79 Å) measured with CDS on-board SOHO, observed on May 30, 2003, and time series of intensity and velocity images from the NSO/Dunn Solar Telescope in the Hα line on September 18, 1994 for the other. The oscillatory content was investigated using Fourier transform and wavelet analysis and compared to different models. Results. In both filaments, oscillations are clearly observed, in intensity and velocity in the He I and Mg X lines, in velocity in Hα, with similar periods from a few minutes up to 80 min, with a main range from 20 to 30 min, simultaneously with eruptions. Both filaments exhibit vertical oscillating motions. For the filament observed in the UV (He I and Mg X lines), we provide evidence of damped velocity oscillations, and for the filament observed in the visible (Hα line), we provide evidence that parts of the filament are oscillating, while the filament is moving over the solar surface, before its disappearance.

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The Coronal Diagnostic Spectrometer for the solar and heliospheric observatory

Cited by 481 publications

References 29 publications

Far- and Extreme-UV Solar Spectral Irradiance and Radiance from Simplified Atmospheric Physical Models

Far- and Extreme-UV Solar Spectral Irradiance and Radiance from Simplified Atmospheric Physical Models

SOHO/SUMER observations and analysis of the hydrogen Lyman spectrum in solar prominences

Oscillatory motions observed in eruptive filaments

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