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Signature of open magnetic field lines in the extended solar corona and of solar wind accelerationThe observations carried out with the ultraviolet coronagraph spectrometer onboard the Solar and Heliospheric Observatory (SOHO) are discussed. The purpose of the observations was to determine the line of sight and radial velocity fields in coronal regions with different magnetic topology. The results showed that the regions where the high speed solar wind flows along open field lines are characterized by O VI 1032 and HI Lyman alpha 1216 lines. The global coronal maps of the line of sight velocity were reconstructed. The corona height, where the solar wind reaches 100 km/s, was determined.
Document ID
19990028046
Document Type
Conference Paper
Authors
Antonucci, E. (Osservatorio Astronomico Turin Italy)
Giordano, S. (Turin Univ. Italy)
Benna, C. (Turin Univ. Italy)
Kohl, J. L. (Harvard-Smithsonian Center for Astrophysics Cambridge, MA United States)
Noci, G. (Florence Univ. Italy)
Michels, J. (Harvard-Smithsonian Center for Astrophysics Cambridge, MA United States)
Fineschi, S. (Harvard-Smithsonian Center for Astrophysics Cambridge, MA United States)
Date Acquired
August 19, 2013
Publication Date
September 1, 1997
Subject Category
Solar Physics
Distribution Limits
Public
Copyright
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