Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...228..246p&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 228, no. 1, Feb. 1990, p. 246-252.
Astronomy and Astrophysics
Astrophysics
29
Doppler Effect, Solar Magnetic Field, Stellar Models, Sunspots, Field Strength, Solar Atmosphere, Zeeman Effect
Scientific paper
From spatially unresolved umbral Stokes-V spectra, magnetic field strength, relative Doppler shift and temperature of a hot and a cool umbral component are investigated. The observed Stokes-V profiles are compared to numerically superposed Stokes-V profiles calculated with various intrinsic model atmospheres and magnetic field parameters and filling factors. An optimal fit is obtained if the temperature of the hot component lies between that of the undisturbed photosphere and 500 K less, whereas the cool component is found to be 350 K hotter than typical models for darkest umbrae suggest. The hot component covers 5 percent of the umbral area observed; this value seems to vary from spot to spot. The magnetic field strength in the hot component is found to be about 20 percent lower than that in the cool component; the magnetic field in both components decreases with height by 2 Gs/km.
Pahlke K.-D.
Wiehr Eberhard
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