Cme and Solar Wind Studies Using Goes Solar X-Ray Imagers and Soho Remote Sensing

  1. J. H. Waite Jr.,
  2. J. L. Burch and
  3. R. L. Moore
  1. W. J. Wagner

Published Online: 18 MAR 2013

DOI: 10.1029/GM054p0279

Solar System Plasma Physics

Solar System Plasma Physics

How to Cite

Wagner, W. J. (1989) Cme and Solar Wind Studies Using Goes Solar X-Ray Imagers and Soho Remote Sensing, in Solar System Plasma Physics (eds J. H. Waite, J. L. Burch and R. L. Moore), American Geophysical Union, Washington, D. C.. doi: 10.1029/GM054p0279

Author Information

  1. Space Environment Laboratory, NOAA/Environmental Research Laboratories, Boulder, CO 80303

Publication History

  1. Published Online: 18 MAR 2013
  2. Published Print: 1 JAN 1989

ISBN Information

Print ISBN: 9780875900742

Online ISBN: 9781118664315



  • Space plasmas;
  • Sun;
  • Magnetosphere;
  • Astrophysics


All inputs to the heliosphere and to planetary magnetospheres and ionospheres are generated in the plasma which constitutes the outer layers of the solar atmosphere. Although the NASA Solar Maximum Mission satellite is expected to re-enter the atmosphere this year, the outlook for observational studies of the solar corona in the mid-1990's looks optimistic. A variety of new instruments will be available for investigations of solar plasma physics processes. Of preeminent importance is the NASA-ESA SOHO satellite, to be stationed at the L1 libration point from 1995. I describe SOHO EUV spectrographic and coronagraphic capabilities for use in identifying these inputs to the magnetosphere as they leave the transition region and high corona. To these data will be added views of launches of coronal mass ejections and the unambiguous locations of soft X-ray coronal holes and magnetic structure in the lower corona. The latter will be recorded by the solar X-ray imagers on the NOAA GOES satellites beginning in 1992 or 1993. I also review the ground-based observational capabilities which are expected to be upgraded in time for the solar cycle maximum campaigns beginning in 1991. The tailoring of the above sensor array to the outstanding problems in mass ejection and coronal research is noted.