Plasma temperature depressions and the open magnetic field-lines model

Details Plasma temperature depressions and the open magnetic field-lines model Plasma temperature depressions and the open magnetic field-lines model

Jun 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981ap%26ss..77..167g&link_type=abstract

Astrophysics and Space Science, vol. 77, no. 1, June 1981, p. 167-178.

Astronomy and Astrophysics

Astrophysics

4

Cold Plasmas, Interplanetary Magnetic Fields, Plasma Temperature, Shock Waves, Solar Corona, Solar Wind, Heat Flux, Magnetic Field Configurations, Solar Corpuscular Radiation, Solar Electrons, Solar Protons, Thermal Conductivity

Scientific paper

It is pointed out that plasma temperature observations in the solar wind at 1 AU show that very low temperatures of electrons and protons appear not only after interplanetary shock waves but also after solar wind streams. The region embedded by a fast preceding and a slower following solar wind is generally believed to be expanding. The plasma inside may thus become cooler. Plasma measurements made aboard the VELA and IMP satellites are discussed. Owing to the limitations of the data, only a qualitative picture is given of the possibility that low temperature regions may be given to local expansions of the plasma. It is also assumed that these regions are not magnetically closed and therefore not thermically isolated but are open and connected with the hot corona along the interplanetary magnetic field lines. These regions are thus heated from the corona as a result of thermal conduction. Attention is given here to both the theoretically predicted and the experimentally measured conducted electron heat fluxes.

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