Doppler shifts of solar UV emission lines and the source region of the (fast) solar wind

Details Doppler shifts of solar UV emission lines and the source region of the (fast) solar wind Doppler shifts of solar UV emission lines and the source region of the (fast) solar wind

Jun 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aipc..471..281p&link_type=abstract

The solar wind nine conference. AIP Conference Proceedings, Volume 471, pp. 281-284 (1999).

Physics

1

Solar Physics, Ultraviolet

Scientific paper

Full-disk observations with the UV spectrograph SUMER on board SOHO offer the possibility to study emission line profiles on the whole solar disk, beyond what was possible in previous UV studies, e.g. with HRTS or on board Skylab. SUMER data acquired during a SOHO spacecraft roll are complementary to the full-disk data as they cover a wider range of emission lines. In both data sets the center-to-limb variation of the Doppler shifts can be studied, allowing a precise determination of the Doppler shift at disk center. The most interesting result is the opposite center-to-limb variation of the lines formed below and above 5.105 K and the blueshift of the hotter lines found at disk center. This is of importance for the understanding of physical models for the transition region from the chromosphere to the corona. By comparing the quiet Sun and coronal hole regions the outflow velocity of the fast solar wind and the variation of the cross-section of the flow channels of the fast solar wind throughout the transition region can be estimated. Finally by comparing different methods of wavelength calibration one can re-evaluate the rest (or ``laboratory'') wavelengths, which are but poorly known for the hotter lines.

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