Astronomy and Astrophysics – Astrophysics
Scientific paper
Jun 1976
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976ap%26ss..41..371p&link_type=abstract
Astrophysics and Space Science, vol. 41, June 1976, p. 371-385.
Astronomy and Astrophysics
Astrophysics
2
Magnetic Field Configurations, Solar Atmosphere, Solar Wind, Topology, Atmospheric Heating, Atmospheric Models, Chromosphere, Fine Structure, Interplanetary Magnetic Fields, Photosphere, Solar Magnetic Field
Scientific paper
The author combines an earlier attempt to develop a magnetically structured solar atmosphere (Piddington, 1972 and 1974) with the idea of Durney and Pneuman that the interplanetary medium should be largely determined by surface fields and that the interplanetary medium should provide information about solar atmospheric fields and plasma. Measured magnetic fields at 1 AU are adopted as a major part of the present model. The solar atmosphere is divided into three regions: (1) an open-field region expanding into the solar wind; (2) a closed-field region from which no plasma may escape; and (3) a nonmagnetic region between and beneath the flux tubes. Transfer of energy and plasma is governed by different processes in the open and closed regions. The solar wind is driven by Alfven waves with enhancements provided by the focusing of acoustic or fast-mode MHD waves. A framework of twisted magnetic fields is proposed to account for complex photospheric and chromospheric fine structure. According to the model, acoustic waves would be insufficient as a source of atmospheric heating, which seems to be explicable only in terms of Alfven waves.
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