The Coronal Diagnostic Spectrometer for the solar and heliospheric observatory |
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| Institution: | (1) Space Science Dept., Rutherford Appleton Laboratory, OX11 0QX Chilton, Didcot Oxfordshire, UK;(2) Mullard Space Science Laboratory, University College London, Holmbury St Mary, RH5 6NT Dorking, Surrey, UK;(3) NASA Goddard Space Flight Center, Code 682, 20771 Greenbelt, MD, USA;(4) Institute of Theroetical Astrophysics, University of Oslo, PO Box 1029, 0315 Blindern, Oslo, Norway;(5) Max- Planck-Institut für Extraterrestrische Physik, D-85748 Garching, Germany;(6) Physikalisch-Technische Bundesanstalt, Inst. Berlin, Abbestrasse 2-12, D-1000 Berlin 10, Germany;(7) Experimental Astrophysics Group, Space Sciences Laboratory, University of California, 94720 Berkeley, CA, USA;(8) ESA, Space Science Dept., ESTEC, PO Box 299, 2200 Noordwijk, AG, The Netherlands;(9) Inst. d'Astrophysique Spatiale, Université Paris XI, 91405 Orsay Cedex, France;(10) Dept. Applied Mathematics and Theoretical Physics, University of Cambridge, CB3 9EW Cambridge, UK;(11) Dept. of Physics and Astronomy, University of Central Lancashire, Preston, PR1 2HE, UK |
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| Abstract: | 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  . 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. Futhermore, coverage of large wavelength bands provides the capability for simultaneously observing the properties of plasmas across the wide temperature ranges of the solar atmosphere. |
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| Keywords: | Solar Atmosphere Extreme UV Spectroscopy |
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