Abstract
Alfvén waves represent one of the most prominent ways of heating the solar corona and accelerating the solar wind. One of their signatures is to broaden the spectral lines in excess of their thermal width. Here we aim to combine observations of non-thermal broadenings measured by SUMER in OVI (1037.6 Å) line and electronic densities derived from white-light observations during the 1998 total eclipse. After checking the validity of the frequently-used assumption of equal ion and electron temperatures, we compute the variation of the non-thermal velocity as a function of height in an interplume region within the south polar coronal hole.
Published Version
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