Investigation of microturbulent magnetic fields in the solar photosphere by their Hanle effect in the SR I 4607 A line

Details Investigation of microturbulent magnetic fields in the solar photosphere by their Hanle effect in the SR I 4607 A line Investigation of microturbulent magnetic fields in the solar photosphere by their Hanle effect in the SR I 4607 A line

Feb 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...268..765f&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 268, no. 2, p. 765-774.

Astronomy and Astrophysics

Astrophysics

73

Photosphere, Solar Magnetic Field, Turbulence Effects, Astronomical Models, Depolarization, Scattering, Solar Limb

Scientific paper

A detailed analysis is made of the center-to-limb variations of the Sr I 4607 A line, recorded by Stenflo et al. (1980). The effect of multiple scattering, depolarizing collisions, and partial frequency redistribution are fully taken into account. We find that the observed polarization rates are hard to explain without depolarizing effects, which following Stenflo (1982) we ascribe to a weak turbulent magnetic field producing depolarization by Hanle effect. As the spatial scale of a weak turbulent magnetic field is likely to be smaller than 300 km, the effect of the turbulent magnetic field is treated in the microturbulent limit. In the transfer equation for the Stokes parameters, the Hanle phase matrix is thus replaced by its average over the magnetic field distribution. We show that the center-to-limb observations of the Sr I 4607 A line polarization indicate the presence in the photosphere of a depth-dependent turbulent magnetic field. Its intensity decreases from values in the range 30 G to 60 G at the altitude z = 150 km above tau 5000 = 1, to values in the range l0 G to 30 G at the altitude z = 250 km. It then remains roughly constant at higher altitudes.

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