Solar maximum ultraviolet spectrometer and polarimeter

Details Solar maximum ultraviolet spectrometer and polarimeter Solar maximum ultraviolet spectrometer and polarimeter

Jan 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979spie..184..264t&link_type=abstract

In: Space optics: Imaging X-ray optics workshop; Proceedings of the Seminar, Huntsville, Ala., May 22-24, 1979. (A80-17469 05-89

Astronomy and Astrophysics

Astronomy

Polarimeters, Solar Instruments, Solar Maximum Mission, Solar Spectrometers, Ultraviolet Spectrometers, Aeronomy, Calibrating, Data Systems, Ebert Spectrometers, Solar Flares, Solar Radiation, Telescopes, Ultraviolet Astronomy

Scientific paper

The objectives of the UVSP experiment are to study solar ultraviolet radiations, particularly from flares and active regions, and to measure constituents in the terrestrial atmosphere by the extinction of sunlight at satellite dawn and dusk. The instrument is designed to observe the Sun at a variety of spectral and spatial resolutions in the range from 1150 to 3600 A. A Gregorian telescope with effective focal length of 1.8 m is used to feed a 1 m Ebert-Fastie spectrometer. A polarimeter containing rotatable magnesium fluoride waveplates is included behind the spectrometer entrance slit and will allow all four Stokes parameters to be determined. Velocities on the Sun can also be measured. The instrument is controlled by a computer which can interact with the data stream to modify the observing program. The observing modes, including rasters, spectral scans, velocity measurements, and polarimetry, are also described along with plans for mission operations, data handling, and analysis of the observations.

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