Topological Changes of the Magnetic Network as Seen in Different UV/EUV Emission Lines

Details Topological Changes of the Magnetic Network as Seen in Different UV/EUV Emission Lines Topological Changes of the Magnetic Network as Seen in Different UV/EUV Emission Lines

Jan 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004esasp.547..169x&link_type=abstract

Proceedings of 'SOHO 13 - Waves, Oscillations and Small-Scale Transient Events in the Solar Atmosphere: A Joint View from SOHO a

Computer Science

Coronal Hole, Magnetic Field, Ultraviolet Radiation

Scientific paper

By combining observations made by SUMER and MDI aboard SOHO, fine structures in equatorial coronal holes have been studied, in particular the relationship between the ultraviolet emission line parameters (line radiance, Doppler shift and line width) and the underlying magnetic field. The bases of coronal holes seen in chromospheric lines generally have similar properties as normal QS regions, i.e., small bright points are the predominant features. An obvious difference has been found in the shape of the H I L line, which has very asymmetric profiles (skewed towards the blue side) in coronal holes. Loop-like structures are the most prominent features in the transition region. In coronal holes, we found that many of such structures seem to have one footpoint rooted in the intra-network and to extend into the cell interiors. Some of them appear as star-shape clusters. In Dopplergrams of the O VI line, there are also fine structures with apparent blue shifts, although on average they are red shifted. Structures with blue shifts have usually also broader line widths. They seem to represent plasma above large concentrations of unipolar magnetic field, without obvious bipolar photospheric magnetic features nearby.

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