Infrared lines as probes of solar magnetic features. I - A many-line analysis of a network region

Details Infrared lines as probes of solar magnetic features. I - A many-line analysis of a network region Infrared lines as probes of solar magnetic features. I - A many-line analysis of a network region

Sep 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...263..301m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 263, no. 1-2, p. 301-311.

Astronomy and Astrophysics

Astrophysics

24

Infrared Spectra, Solar Magnetic Field, Line Spectra, Magnetic Flux, Radiative Transfer, Solar Atmosphere, Stellar Models, Zeeman Effect

Scientific paper

The results are presented of an analysis of a Fourier transform spectrometer Stokes I and V spectrum in the H band of a solar network region. From a many-line statistical analysis of the measured Stokes F profiles, it is concluded that there is no evidence for s systematic up or downflow greater than 200-300 m/s within the magnetic element of the observed region. The Stokes V profiles in the H band show a blue-red asymmetry having the same sign as in the visible, but a smaller magnitude. The lines with g(eff) greater than about 1.5 are more or less completely Zeeman split in the observed region, and only lines with g(eff) values well below unity can be considered to be in the weak-field regime. An analysis based on radiative transfer calculations of 16 selected spectral lines in a flux tube model shows that a thin tube with a field strength of 2050 G at tau (1.6) = 1 , corresponding to 1500 G at z = 0, fits the profiles best.

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