Computer Science
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...3e..87z&link_type=abstract
Solar Active Regions and 3D Magnetic Structure, 26th meeting of the IAU, Joint Discussion 3, 16-17 August, 2006, Prague, Czech R
Computer Science
Scientific paper
High-resolution spectroscopic observations of the Sun have been carried out with the TRIPPEL spectrograph installed at the new 1-m Swedish Solar Telescope (SST) using realtime AO correction. A detailed spectroscopic analysis of individual photospheric bright points (BP) and faculae-like structures simultaneously in two spectral domains, i.e 387.588<λ<388.473 nm (violet CN band) and in a blue spectral band at 436.1<λ<436.9 nm, containing absorption lines of CH, obtained at the disc center and near the limb is presented. The estimated spatial resolution of the obtained spectra is around 0.25 arcsec while the spectral resolving power is around 130.000 in the first domain, and 76.000 in the second spectral region, respectivlely. The first spectral band covers absorption lines of both, CH and CN molecules, as well as many atomic lines. This enabled us to make a quantitative comparison of their absorption and Doppler shifts in the different photospheric features. The absorption lines of the CN molecule and many atoms are depressed in a BP's interior with respect to those in the quiet Sun. Our quantitative comparison of the relative line depression of CH lines with respect to CN lines showed that the latter have weaker absorption by a factor of 1.28 at the disc centre and 1.32 near the limb. The CN line-core intensity, at the disc centre, has higher BP contrast than the contrast in the CH line-core by a factor of 1.9, and the ratio of these contrasts is decreasing with increasing continuum intensity of the BPs. This trend is similar to that obtained from previous simultaneous G-band and violet CN-band imaging observations. Measurements of contrasts and rms contrasts of line-core, integrated and local continuum intensities are provided. Analysis of Doppler shifts and line broadening of an Fe I line at 387.777 nm revealed an increase of the FWHM in the BP's interior and in dark intergranular lanes and a decrease with increasing intensity of the granules. The first results of a direct comparison of observed CN spectra with those simulated in MHD models in different photospheric features is presented.
Gandorfer Achim
Solanki Sami K.
Zakharov Valentin
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