Spectroscopic Studies of Steady Coronal Structures -- Line Width Variations with Height of Ion{Fe{X-XIV}} Emission Lines

Details Spectroscopic Studies of Steady Coronal Structures -- Line Width Variations with Height of Ion{Fe{X-XIV}} Emission Lines Spectroscopic Studies of Steady Coronal Structures -- Line Width Variations with Height of Ion{Fe{X-XIV}} Emission Lines

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aspc..325..235s&link_type=abstract

The Solar-B Mission and the Forefront of Solar Physics, ASP Conference Series, Vol. 325, Proceedings of the Fifth Solar-B Scienc

Physics

Scientific paper

We have obtained spectrographic observations of several steady coronal structures at the limb overlying the sunspot regions on several days in ion{Fe{x-xiv}} emission lines. The line-width measurements indicate that in steady coronal structures the FWHM of the 6374 AA line increases with height above the limb with an average value of 1.02 mAA per arcsec. Whereas the FWHM of the 5303 AA line decreases with an average value of -0.66 mAA per arcsec. The FWHM of the 7892 AA and 10747 AA lines increases with values of 0.55 and 0.29 mAA per arcsec, respectively. We find that FWHM of emission lines in coronal structures increases with height if the associated ionization temperature is less than 1.6 MK, with gradient depending upon the ionization temperature of the line, while the FWHM decreases with height for lines whose ionization temperature is greater than 1.6 MK. It implies that it may not always be possible to interpret the observed increase in FWHM with height in terms of an increase in the non-thermal velocity. To investigate further, we propose simultaneous observations in number of EUV lines with EIS onboard SolarB and in ion{Fe{x-xiv}} in the visible wavelengths with the 25-cm coronagraph at Norikura.

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