The Ultraviolet Coronagraph Spectrometer for the Solar and Heliospheric Observatory

TitleThe Ultraviolet Coronagraph Spectrometer for the Solar and Heliospheric Observatory
Publication TypeJournal Article
Year of Publication1995
AuthorsKohl, J. L., Esser R., Gardner L. D., Habbal S., Daigneau P. S., Dennis E. F., Nystrom G. U., Panasyuk A., Raymond J. C., Smith P. L., Strachan L., van Ballegooijen A. A., Noci G., Fineschi S., Romoli M., Ciaravella A., Modigliani A., Huber M. C. E., Antonucci E., Benna C., Giordano S., Tondello G., Nicolosi P., Naletto G., Pernechele C., Spadaro D., Poletto G., Livi S., von der Lühe O., Geiss J., Timothy J. G., Gloeckler G., Allegra A., Basile G., Brusa R., Wood B., Siegmund O. H. W., Fowler W., Fisher R., and Jhabvala M.
JournalSolar Physics
Date PublishedDec

The SOHO Ultraviolet Coronagraph Spectrometer (UVCS/SOHO) is composed of three reflecting telescopes with external and internal occultation and a spectrometer assembly consisting of two toric grating spectrometers and a visible light polarimeter. The purpose of the UVCS instrument is to provide a body of data that 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 primary scientific goals are the following: to locate and characterize the coronal source regions of the solar wind, to identify and understand the dominant physical processes that accelerate the solar wind, to understand how the coronal plasma is heated in solar wind acceleration regions, and to increase the knowledge of coronal phenomena that control the physical properties of the solar wind as determined byin situ measurements. To progress toward these goals, the UVCS will perform ultraviolet spectroscopy and visible polarimetry to be combined with plasma diagnostic analysis techniques to provide detailed empirical descriptions of the extended solar corona from the coronal base to a heliocentric height of 12 solar radii.