Other
Scientific paper
Jun 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995injpb..69..187a&link_type=abstract
Indian J. Phys., Part B, Vol. 69B, No. 3, p. 187 - 218
Other
Solar Corona: Magnetic Fields, Solar Wind: Heliosphere
Scientific paper
Although the spacecraft observations made three decades ago revealed the highly structured nature of the solar corona, its three-dimensional aspects in the heliosphere become known as a result of the highly successful spacecraft missions of the Skylab and the twin Helios. It is well known now that the magnetic field, corona and solar wind are strongly related to one another and that their structures vary considerably with the sunspot cycle. Particularly, the solar magnetic field strongly influences the shape of the corona and determines the inner boundary conditions which must be satisfied for the escape of the solar wind. Applying a potential field-source surface model to the photospheric field data, the configurations of the coronal and heliospheric fields are computed. These calculations enable mapping of open-field and closed-field coronal regions that coincide with known coronal holes and active solar regions respectively. The purpose of this overview is to present these developments briefly and highlight their inter-relations for understanding the heliospheric phenomena. It begins with observational background which preceded Parker's ingenious suggestion of a spherically symmetric, continuous coronal expansion - the solar wind. The salient features of his hydrodynamic model are recalled, with limitations of the expansion speed of the thermally-driven plasma flow. Recent theoretical developments of the solar wind acceleration mechanism which overcome these speed limitations are briefly summarized.
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