Electric fields in coronal magnetic loops

Details Electric fields in coronal magnetic loops Electric fields in coronal magnetic loops

Feb 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983soph...83...83f&link_type=abstract

Solar Physics, vol. 83, Feb. 1983, p. 83-102.

Physics

17

Balmer Series, Coronal Loops, Electric Fields, Solar Flares, Solar Magnetic Field, Stark Effect, Electron Density (Concentration), Plasma Dynamics, Solar Prominences, Solar Spectra, Spectrum Analysis

Scientific paper

The present search for evidence of Stark effect on Balmer lines formed in coronal structures, through the analysis of spectra taken with a 40-cm coronograph, has uncovered significant broadening from H(10) to the limit of Balmer line visibility at about H(20) in spectra taken near the apex of a bright, post-flare loop prominence. This increasing width is interpreted as Stark broadening. The trend observed in one post-flare loop requires an ion density of 2 x 10 to the 12th/cu cm, if it is to be explained entirely as Stark effect caused by pressure broadening. A comparison of evidence from electron scattering with densities derived from emission features and line intensity ratios is adduced as evidence against a volume filling factor small enough to reconcile the ion density and mean electron density derived in the present study, suggesting that the Stark effect observed in the loops could be caused by macroscopic electric fields rather than pressure broadening.

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