Solar magnetic field strength determinations from high spatial resolution filtergrams

Details Solar magnetic field strength determinations from high spatial resolution filtergrams Solar magnetic field strength determinations from high spatial resolution filtergrams

Sep 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...236..250k&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 236, no. 1, Sept. 1990, p. 250-255.

Astronomy and Astrophysics

Astrophysics

18

Filtergrams, Magnetic Flux, Solar Activity, Solar Magnetic Field, Circular Polarization, High Resolution, Lines Of Force, Spatial Resolution

Scientific paper

Circularly polarized images with high spatial resolution (better than 1 arcsec) of a solar active region, obtained with a tunable filter in the wings of Fe I 5247.1 A and Fe I 5250.2 A, have been analyzed in terms of the magnetic line ratio technique introduced by Stenflo (1973). Whenever a measurable amount of polarization is present, the distribution of the observed magnetic-line ratio is compatible with a unique value, which is randomly blurred by noise due to the photon statistics, the CCD camera, and atmospheric distortions. There is no need for a distribution of field strengths to explain the observed distribution of the magnetic line ratio. Consequently, the observations are compatible with a unique magnetic field strength in solar small-scale magnetic elements of about 1000 G at the level of line formation. For a thin flux tube, this corresponds to a field strength of approximately 2000 G at the level of continuum formation, which is in excellent agreement with previous field strength determinations from low spatial resolution spectra (4-10 arcsec).

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