Core, Halo and Strahl Electrons in the Solar Wind

Details Core, Halo and Strahl Electrons in the Solar Wind Core, Halo and Strahl Electrons in the Solar Wind

Jun 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001ap%26ss.277..195p&link_type=abstract

Astrophysics and Space Science, v. 277, Issue 1/2, p. 195-200 (2001).

Astronomy and Astrophysics

Astrophysics

7

Scientific paper

Electron velocity distribution functions (VDF) observed in the low speed solar wind flow are generally characterized by ‘core’ and ‘halo’ electrons. In the high speed solar wind, a third population of ‘strahl’ electrons is generally observed. New collisional models based on the solution of the Fokker-Planck equation can be used to determine the importance of the different electron populations as a function of the radial distance. Typical electron velocity distribution functions observed at 1 AU from the Sun are used as boundary conditions for the high speed solar wind and for the low speed solar wind. Taking into account the effects of external forces and Coulomb collisions with a background plasma, suprathermal tails are found to be present in the electron VDF at low altitudes in the corona when they exist at large radial distances.

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