Solar Physics

, Volume 162, Issue 1, pp 313–356

The Ultraviolet Coronagraph Spectrometer for the solar and heliospheric observatory

Authors

  • J. L. Kohl
    • Harvard-Smithsonian Center for Astrophysics
  • R. Esser
    • Harvard-Smithsonian Center for Astrophysics
  • L. D. Gardner
    • Harvard-Smithsonian Center for Astrophysics
  • S. Habbal
    • Harvard-Smithsonian Center for Astrophysics
  • P. S. Daigneau
    • Harvard-Smithsonian Center for Astrophysics
  • E. F. Dennis
    • Harvard-Smithsonian Center for Astrophysics
  • G. U. Nystrom
    • Harvard-Smithsonian Center for Astrophysics
  • A. Panasyuk
    • Harvard-Smithsonian Center for Astrophysics
  • J. C. Raymond
    • Harvard-Smithsonian Center for Astrophysics
  • P. L. Smith
    • Harvard-Smithsonian Center for Astrophysics
  • L. Strachan
    • Harvard-Smithsonian Center for Astrophysics
  • A. A. Van Ballegooijen
    • Harvard-Smithsonian Center for Astrophysics
  • G. Noci
    • Università di Firenze
  • S. Fineschi
    • Università di Firenze
  • M. Romoli
    • Università di Firenze
  • A. Ciaravella
    • Università di Firenze
  • A. Modigliani
    • Università di Firenze
  • M. C. E. Huber
    • Space Science Dept.ESA/ESTEC
  • E. Antonucci
    • Università di Torino
  • C. Benna
    • Università di Torino
  • S. Giordano
    • Università di Torino
  • G. Tondello
    • Università di Padova
  • P. Nicolosi
    • Università di Padova
  • G. Naletto
    • Università di Padova
  • C. Pernechele
    • Università di Padova
  • D. Spadaro
    • Osservatorio Astrofisico di Catania
  • G. Poletto
    • Osservatorio Astrofisico di Arcetri
  • S. Livi
    • Max Planck Institut für Aeronomie
  • O. Von Der Lühe
    • European Southern Observatory
  • J. Geiss
    • International Space Science Institute
  • J. G. Timothy
    • University of New Brunswick
  • G. Gloeckler
    • University of Maryland
  • A. Allegra
    • Alenia Spazio
  • G. Basile
    • Officine GalileoDivisione Ottica e Spazio
  • R. Brusa
    • Brusag
  • B. Wood
    • Oerlikon-ContravesSpace Division
  • O. H. W. Siegmund
    • Space Sciences LaboratoryUniversity of California
  • W. Fowler
    • Ball CorporationElectro-Optics and Cryogenics Div.
  • R. Fisher
    • NASA/Goddard Space Flight Center
  • M. Jhabvala
    • NASA/Goddard Space Flight Center
Article

DOI: 10.1007/BF00733433

Cite this article as:
Kohl, J.L., Esser, R., Gardner, L.D. et al. Sol Phys (1995) 162: 313. doi:10.1007/BF00733433

Abstract

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.

Key words

SunSolar CoronaSolar WindUV SpectroscopyUV Coronagraph
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Copyright information

© Kluwer Academic Publishers 1995