Electron heating by fast mode magnetohydrodynamic waves in the solar wind emanating from coronal holes

Details Electron heating by fast mode magnetohydrodynamic waves in the solar wind emanating from coronal holes Electron heating by fast mode magnetohydrodynamic waves in the solar wind emanating from coronal holes

Feb 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...253..318h&link_type=abstract

Astrophysical Journal, Part 1, vol. 253, Feb. 1, 1982, p. 318-322. Research supported by the Norges Teknisk-Naturvitenskapelige

Astronomy and Astrophysics

Astrophysics

33

Coronal Holes, Electron Energy, Magnetohydrodynamic Waves, Plasma-Particle Interactions, Propagation Modes, Solar Wind, Collisionless Plasmas, Energy Dissipation, Proton Energy, Radiant Flux Density

Scientific paper

It is shown that fast mode magnetohydrodynamic waves, propagating outwards from the sun in coronal hole regions, will dissipate primarily through collisionless interaction with electrons rather than with protons. This dissipation can lead to higher electron than proton temperatures in the accelerating region of the solar wind, provided the waves carry a sufficiently large energy flux.

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