Coronal mass ejections: The long-term variation of their occurrence rate and the solar wind mass flux

Details Coronal mass ejections: The long-term variation of their occurrence rate and the solar wind mass flux Coronal mass ejections: The long-term variation of their occurrence rate and the solar wind mass flux

Sep 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987sici.symp...26w&link_type=abstract

In Alabama Univ., Huntsville. STIP Symposium on Physical Interpretation of Solar/Interplanetary and Cometary Intervals p 26 (SEE

Physics

Flux (Rate), Interplanetary Medium, Intervals, Solar Corona, Solar Wind, Stellar Mass Ejection, Coronagraphs, Helios Project, Photometers, Skylab Program, Solar Activity, Solar Flares, Solar Maximum Mission, White Light Holography

Scientific paper

Solar Coronal Mass Ejections (CMEs) from the Sun are an important aspect of coronal physics, and a potentially important contributor to the solar wind mass flux. However, despite significant progress in studies of CMEs since their discovery in the early 70's, questions remain about their effects on the interplanetary medium. A study is done of the long-term variations of the occurrence rates of CMEs, of activity tracers related to CMEs, and of the solar wind particle flux. CMEs are most directly detected by scattered electron radiation in white light. To estimate their long-term occurrence frequency and their contributions to the in-ecliptic solar wind mass flux, observed CME rates must be corrected for instrumental duty cycles, detection efficiency out of the plane of the sky, mass detection thresholds, and geometrical considerations. These corrections are evaluated using data on solar CMEs from the spaceborne Skylab, SMM, and SOLWIND coronagraphs and on interplanetary plasma clouds from the HELIOS white light photometers. Variations in the CME rate and the contribution of CMEs to the solar wind mass flux are traced over nearly a complete solar activity cycle.

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