The solar wind

Details The solar wind The solar wind

May 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987esasp.268..131s&link_type=abstract

In ESA Space Astronomy and Solar System Exploration p 131-141 (SEE N87-29374 23-88)

Astronomy and Astrophysics

Astronomy

2

Solar Wind, Solar Wind Velocity, Stellar Models, Galactic Cosmic Rays, Solar Activity Effects, Solar Corona, Solar Cycles, Solar Flares

Scientific paper

Parker's theoretical model of the solar wind, i.e., a continuous outflow of particles from the solar corona is found to be in basic agreement with observations. More sophisticated models and more detailed measurements reveal significant gaps in understanding. The high values of flow speed in high speed streams cannot be explained, and identifying coronal sources of the slow solar wind reveals severe topological problems. It appears as if there are basic differences in the acceleration mechanism for slow and fast solar wind. The variation of the average solar wind during the solar activity cycle is only a minor effect. Modulation of galactic cosmic radiation by solar activity is probably due to transient effects on the Sun. Coronal mass ejections in association with solar flares or eruptive prominences drive interplanetary shock waves into the solar wind throughout the heliosphere. However, there are gaps in understanding of reactions between the Sun's surface and the outer solar system.

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