Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004a%26a...423.1147l&link_type=abstract
Astronomy and Astrophysics, v.423, p.1147-1157 (2004)
Astronomy and Astrophysics
Astrophysics
7
Sun: Photosphere
Scientific paper
A detailed analysis of high-resolution spectra obtained in three different wavelength regions (at 430 nm, 526 nm and 569 nm) of G-band bright points in the solar photosphere is presented. They show an average intensity contrast of 11% with respect to the ``quiet'' sun reference. The CH lines are weakened in the bright point interior. The atomic lines, too, e.g. the Fe I line at 569.15 nm, weaken in the bright point interior. In contrast thereto, the absorption line of single ionized iron at 526.48 nm remains almost constant between bright point interior and the immediate surroundings. Line-of-sight velocities show a stronger downflow within bright points than in the close environment. A net downflow relative to the intergranular surroundings of around 80 m/s is measured. Filling factors are calculated from a comparison with synthesized spectra for different flux tube models and are used to estimate the ``true'' velocity in bright points with respect to their immediate surroundings. We obtain up- and downflows in the order of one km s-1, in agreement with the magneto-convective picture of the formation and dispersal of magnetic flux tubes. From the different behavior of the metallic lines and the CH lines we conclude that the line-weakening process that leads to the G-band bright points is mainly due to hot-wall radiation. This confirms that these bright points are indeed magnetic flux elements.
Langhans Kai
Rimmele Th.
Schmidt Wolfram
No associations
LandOfFree
Diagnostic spectroscopy of G-band brightenings in the photosphere of the sun does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Diagnostic spectroscopy of G-band brightenings in the photosphere of the sun, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Diagnostic spectroscopy of G-band brightenings in the photosphere of the sun will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1059239