The Expansion of Coronal Plumes in the Fast Solar Wind

Details The Expansion of Coronal Plumes in the Fast Solar Wind The Expansion of Coronal Plumes in the Fast Solar Wind

May 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998ssrv...85..349d&link_type=abstract

Space Science Reviews, v. 85, Issue 1/2, p. 349-356 (1998).

Physics

7

Mhd, Sun: Corona, Sun: Coronal Plumes, Solar Wind, Fip-Effect

Scientific paper

Coronal plumes are believed to be essentially magnetic features: they are rooted in magnetic flux concentrations at the photosphere and are observed to extend nearly radially above coronal holes out to at least 15 solar radii, probably tracing the open field lines. The formation of plumes itself seems to be due to the presence of reconnecting magnetic field lines and this is probably the cause of the observed extremely low values of the Ne/Mg abundance ratio.

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