Nonlinear Waves and Chaos in Space Plasmas UVCS observations(3.4)


Line widths

Line widths and empirical most-probable speeds for HI and OVI derived from emission line profiles measured with UVCS above polar coronal hole.

 H speeds parallel to the radial magnetic field (yellow) may be as large as the speeds in the perpendicular direction (green).

 O speeds above about 2.2 solar radii => the parallel speeds (blue) are constrained by Doppler-dimmed intensity ratios to be decisively smaller than the perpendicular speeds (red)