The Coronal Diagnostic Spectrometer for the solar and heliospheric observatory

• Published in: Solar physics 1995-12, Vol.162 (1-2), p.233-290
• Main Authors: Harrison, R. A., Sawyer, E. C., Carter, M. K., Cruise, A. M., Cutler, R. M., Fludra, A., Hayes, R. W., Kent, B. J., Lang, J., Parker, D. J., Payne, J., Pike, C. D., Peskett, S. C., Richards, A. G., Gulhane, J. L., Norman, K., Breeveld, A. A., Breeveld, E. R., Al Janabi, K. F., Mccalden, A. J., Parkinson, J. H., Self, D. G., Thomas, P. D., 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.
• Format: Article
• Language: English
• ISSN: 0038-0938; 1573-093X
• DOI: 10.1007/BF00733431

The Coronal Diagnostic Spectrometer is designed to probe the solar atmosphere through the detection of spectral emission lines in the extreme ultraviolet wavelength range 150-800 A. By observing the intensities of selected lines and line profiles, we may derive temperature, density, flow and abundance information for the plasmas in the solar atmosphere. Spatial and temporal resolutions of down to a few arcseconds and seconds, respectively, allow such studies to be made within the fine-scale structure of the solar corona. Furthermore, coverage of large wavelength bands provides the capability for simultaneously observing the properties of plasmas across the wide temperature ranges of the solar atmosphere.