Coronal Hole Diagnostics out to 8 solar radii

Details Coronal Hole Diagnostics out to 8 solar radii Coronal Hole Diagnostics out to 8 solar radii

Oct 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999esasp.446..281d&link_type=abstract

8th SOHO Workshop: Plasma Dynamics and Diagnostics in the Solar Transition Region and Corona. Proceedings of the Conference hel

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

The line width measurements (from Si VIII) and Ne estimates (from Si VIII and Si IX) based on SUMER and CDS observations are combined with LASCO and UVCS output to provide an overview of its variations with height above a polar coronal hole. From the combined dataset we find a radial dependence of the electron density, in the range 1-2 solar radii as r-8, from 2 to 4 solar radii as r-4 and then as r-2. Combining the Si VIII half width at 1/e of the peak intensity with the UVCS O VI half width, we find a small increase of the half width from 1 to 1.2 solar radii, then a plateau until 1.5 solar radii, thereafter a sharp increase until 2 solar radii, finally a more gradual increase reaching 550 km/s at 3.5 solar radii. Our data suggests that the MHD waves responsible for the excess line broadening tends to become non-linear as it reaches 1.2 solar radii.

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