The origin of noncompressive density enhancements in the solar wind

Details The origin of noncompressive density enhancements in the solar wind The origin of noncompressive density enhancements in the solar wind

Dec 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983azh....60.1196k&link_type=abstract

(Astronomicheskii Zhurnal, vol. 60, Nov.-Dec. 1983, p. 1196-1203) Soviet Astronomy (ISSN 0038-5301), vol. 27, Nov.-Dec. 1983, p.

Astronomy and Astrophysics

Astronomy

Plasma Density, Solar Corona, Solar Magnetic Field, Solar Wind, Interplanetary Magnetic Fields, Magnetic Field Configurations, Solar Protons

Scientific paper

A model is proposed according to which noncomrpessive density enhancements are formed in regions of the corona with converging magnetic field configurations. The model makes it possible to understand the reasons for the high density and low temperature of noncompressive enhancements, as well as to explain the variation of their characteristics during a solar activity cycle and their connection with the boundaries of sectors of the interplanetary magnetic field. It is established that noncompressive density enhancements make a significant contribution to the balance of mass and energy of the solar wind at 1 AU during the decline and minimum of solar activity.

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