Abstract
The magnetic splitting peculiarities of the absorption lines in the sunspot spectrum are considered. The most common and typical of them is breaking of all Stokes parameter symmetry in regard to the line center. The possible reason of this effect is the macroscopic gas motion with inhomogeneous velocity. Computed contours are given for the line Fe i λ5250 Å with various combinations of magnetic and velocity fields. Magneto-optical effects within the line which are connected with the magnetic and velocity field inhomogeneity are discussed. The observation results are discussed for longitudinal magnetic field zero lines. These observations were carried out for the sunspot and photosphere in two spectral lines Fe i λλ 5250 and 5233 Å. In the sunspot the regular displacement of one zero line with respect to the other zero line takes place whereas in the photosphere the displacements are random. The possible reason of the regular displacement is the change of the magnetic field direction in the different optical layers wherein corresponding spectral lines are formed effectively. The connection between the zero line displacement of a longitudinal magnetic field and the crossover effect is discussed. The computation results are given which agree with observations and illustrate the above-mentioned relationship. The influence of the Stokes parameter asymmetry on the measured magnetic field signals is considered.
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References
Beckers, J. M.: 1969, Solar Phys. 9, 372.
Bumba, V.: 1962, Bull. Astron. Inst. Czech. 13, 42.
Deubner, F. L.: 1967, Mitt. Astron. Ges. 22, 33.
Gingerich, O. and De Jager, C.: 1968, Solar Phys. 3, 5.
Golovko, A. A.: 1974, Solar Phys. 37, 113.
Grigorjev, V. M. and Katz, J. M.: 1972, Solar Phys. 22, 119.
Henoux, J. C.: 1968, Solar Phys. 4, 315.
Katz, J. M.: 1972, Solar Phys. 24, 28.
Katz, J. M.: 1973, Issledovanija po Geomagnetizmu, Aeronomii i Fizike Solntsa (U.S.S.R.), 28, 67.
Kjeldseth Moe, O. : 1967, in K. O. Kiepenheuer (ed.), ‘Structure and Development of Solar Active Regions’, IAU Symp. 35, 202.
Kuznetsov, D. A., Kuklin, G. V., and Stepanov, V. E.: 1966, Result, nabl. i issled. v period MGSS (U.S.S.R.), 1, 80.
Lisitsa, S. G. and Tshystjakov, V. F.: 1970, Astron. Zirk. (U.S.S.R.), No. 548.
Livingston, W. and Harvey, J. : paper presented at AAS Special Meeting on Solar Astronomy, Boulder, Colorado, October, 1966.
Matta, F. and Reichel, A.: 1971, Mathematics of Computation 25, No. 114. 339.
Mehltretter, J. P.: 1969, Solar Phys. 9, 387.
Mogilevsky, E. I.: 1968, Geodät. Geophys. Veröffentl. Ser. 11, No. 13, 95.
Rachkovsky, D. N.: 1972, Izv. Krymsk. Astrofiz. Obs. 44, 64.
Severny, A. B.: 1959, Astron. Zh. 36, 208.
Staude, J.: 1969, Solar Phys. 8, 264.
Staude, J.: 1970, Solar Phys. 15, 102.
Staude, J.: 1973, Solar Phys. 32, 403.
Wittmann, A.: 1972, Mitt. Astron. Ges. 31, 150.
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Grigorjev, V.M., Katz, J.M. Magnetoactive lines in the medium with the velocity gradient. Sol Phys 42, 21–35 (1975). https://doi.org/10.1007/BF00153280
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DOI: https://doi.org/10.1007/BF00153280