Origin of the solar wind and coronal mass ejections

Details Origin of the solar wind and coronal mass ejections Origin of the solar wind and coronal mass ejections

Sep 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992esasp.346..205s&link_type=abstract

In ESA, Study of the Solar-Terrestrial System p 205-206 (SEE N93-31674 12-90)

Physics

Ejecta, Heliosphere, Plasma Heating, Solar Activity Effects, Solar Corona, Solar Wind, Stellar Mass Ejection, Flux Density, Helium, High Speed, Solar Physics

Scientific paper

Theories on the origin of solar wind, theories that are derived from Parker's first theory on the existence and evolution of solar wind, are discussed. It is suggested that knowledge on how the corona is heated would lead to insight into the problem of solar wind acceleration. From observations of solar wind stream structure through almost three solar activity cycles, four different types of solar wind and their respective coronal sources have been discerned. Each of these are discussed: high speed wind in highspeed streams, low speed wind of the 'interstream' type, low speed wind of the 'maximum' type, and coronal mass ejecta following interplanetary shocks. For each type of solar wind, the following parameters are given: high speed, low density, low particle flux, helium content, and source. A list of the most urgent questions in context with the solar wind origin is given.

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