Astronomy and Astrophysics – Astrophysics
Scientific paper
Nov 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...278..584w&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 278, no. 2, p. 584-588
Astronomy and Astrophysics
Astrophysics
21
Solar Magnetic Field, Solar Spectra, Sunspots, Calcium, Doppler Effect, Iron, Landau Factor, Line Spectra, Zeeman Effect
Scientific paper
Stokes-V and I spectra of sunspot structures have been observed simultaneously in the lines Fe 6843 and Ca 6103 originating from layers which differ by more than 350 km. The Fe line is totally split thus allowing to deduce the field strength from the Stokes-I and V profiles. Both splitting values yield a field strength reduction up to 20% in brighter (peripheral) dots at the umbral border. This reduction is not seen in the higher layer where the Ca line originates. The faint (central) dots do not exhibit a field strength difference with respect to their darker surroundings. Using the ratio of pi to sigma depressions of the totally split Fe 6843 line as a measure for the field inclination, the field lines are found to be essentially flatter in a light bridge than in its neighborhood. Flatter fields are also found in some of the peripheral dots. The Doppler shifts of the Fe and of the Ca line deviate significantly from each other but do not show a relation to the umbral structures.
Degenhardt Detlev
Wiehr Eberhard
No associations
LandOfFree
Magnetic field strengths in umbral dots 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 Magnetic field strengths in umbral dots, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Magnetic field strengths in umbral dots will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-807238