Cooling of solar wind electrons inside 0.3 AU

Details Cooling of solar wind electrons inside 0.3 AU Cooling of solar wind electrons inside 0.3 AU

Jun 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989jgr....94.6893m&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 94, June 1, 1989, p. 6893-6898.

Physics

44

Cooling, Electron Energy, Solar Electrons, Solar Wind, Helios Satellites, Interplanetary Space, Temperature Gradients

Scientific paper

Mean temperature gradients of solar wind electrons between 0.3 and 1 AU are determined from Helios observations. Electrons are found to cool more slowly than adiabatically, with flattest temperature profiles in high-speed streams. These in situ observations are used to estimate the radial gradients of Te inside 0.3 AU under the constraint of matching coronal temperatures. Electrons in high-speed streams are inferred to cool more strongly closer to the sun than within the Helios orbital range. For low-speed wind, no significant breaks in the temperature profiles have been found, while for intermediate-speed structures the results are somewhat ambiguous. These results are discussed in the context of solar wind generation and modeling.

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