Other
Scientific paper
Apr 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003kfnt...19..107s&link_type=abstract
Kinematika i Fizika Nebesnykh Tel, vol. 19, no. 2, p. 107-125
Other
6
Scientific paper
We obtained the distribution of the strength of magnetic fields at various levels of the quiet Sun's photosphere on the basis of the 2-D MHD simulation of magnetogranulation and from the synthesis of |V| profiles maxima of the line Fe I λ 1564.8 nm. The shape of the distribution and its maximum position vary essentially with depth. The distribution maximum is, on the average, about 25 mT. The distribution maximum is close to 35 mT if the spatial average of profiles (about 0.5'') is taken into account. A difference between obtained distributions is caused by errors of the determination of the strength of a field from splitting of V profiles. Our analysis of the method errors shows that the use of the line λ 1564.8 nm in this method provides the most effective and reliable way for measuring fields above 50 mT when the line is in the strong splitting regime. In the weak splitting regime (lower than 17 mT) measured field strengths are equal to about 20 mT, and in an intermediate regime they are overestimated by 2--4 mT. Distribution found with the help of line λ 1564.8 nm can be used as a standard for the testing of other approaches and lines in the region of fields with B > 50 mT. The results of the analysis of synthesized profiles of the iron line λ 630.2 nm confirm that this line is less suitable for the study of the field strength distribution because of its weak magnetic sensitivity to fields below 120 mT. Besides, the inclination of the vector of a magnetic field influences strongly the separation of σ components of this line. The effect of additional separation of V peaks with increasing the inclination angle leads to an essential (about 20--30 mT) overestimation of the strength of weak inclined fields determined by the methods which do not take into account the Q, U profiles. Our distributions of magnetic fields as well as the distribution of asymmetry parameters and V profiles zero-crossing, firstly, agree satisfactorily with infrared observations. Secondly, they confirm convincingly an assumption on a continuous spectrum of structures and values of strength of magnetic photospheric field with mixed polarity down to the scales considerably smaller than a resolution threshold. Thirdly, our distributions indicate that the structure and the scales of magnetic fields are closely connected to the granulation structure.
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