Heating of the interstellar medium by the solar wind

Details Heating of the interstellar medium by the solar wind Heating of the interstellar medium by the solar wind

Oct 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983p%26ss...31.1157k&link_type=abstract

Planetary and Space Science (ISSN 0032-0633), vol. 31, Oct. 1983, p. 1157-1164.

Computer Science

6

Interstellar Gas, Solar Wind, Elastic Scattering, Gas Heating, Solar Protons, Temperature Distribution

Scientific paper

The heating of inflowing interstellar gas by the solar wind is calculated. The experimental differential cross sections have been used for calculating electron-H (He) and proton-H (He) elastic scattering rate coefficients. The solar wind is assumed to be a two-component (protons and electrons), steady, spherically symmetric stream moving radially outward, with the inflowing gas following Keplerian trajectories. The spatial distributions of effective temperature increase within interplanetary space have been obtained.

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