Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.3308k&link_type=abstract
American Astronomical Society, 180th AAS Meeting, #33.08; Bulletin of the American Astronomical Society, Vol. 24, p.781
Astronomy and Astrophysics
Astrophysics
Scientific paper
The purpose of the Ultraviolet Coronagraph Spectrometer (UVCS) is to provide information about the behavior, in the extended corona, of the primary particles (protons and electrons) and several minor ions (O(5+) , Mg(9+) , Si(11+) , and Fe(11+) ). Spectroscopic diagnostic techniques will be used to determine random velocity distributions, densities, and bulk outflow velocities for these particles. The resulting empirical description of the extended corona can be used to address a broad range of scientific questions regarding the nature of the solar corona and the generation of the solar wind. The instrument consists of an externally and internally occulted telescope assembly and a spectrometer assembly. It has three channels whose purposes are the following: 1) VUV spectroscopy and absolute radiometry in the 1130 to 1361 Angstroms wavelength range with spectral resolution up to 9800 and spatial resolution elements of 7" or larger, 2) EUV spectroscopy and absolute radiometry in the 937 to 1127 Angstroms (first order) and 469 to 655 Angstroms (second order) wavelength ranges with spectral resolution up to 12000 and the same spatial resolution as the VUV channel, and 3) White light polarimetry with a wavelength band pass of 4500 -- 6000 Angstroms and a single 14" by 14" spatial resolution element. MAMA detectors provide simultaneous ultraviolet observations of a 40' long strip (parallel to a limb tangent) of the corona. Mirror and instrument motions allow this instantaneous field-of-view to scan out to heliocentric heights of 10 Rsun and onto the solar disk. This work is supported by NASA under contract NAS5-31250 to the Smithsonian Astrophysical Observatory.
Kohl John L.
Noci Giancarlo
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