Abstract
The velocity field in a large complex sunspot is investigated in Fe i λ 6302.5 Å and in Hα with a spatial resolution of about 2.5″. The Evershed flow is almost parallel to the solar surface. For the inclination angle θ between the velocity and the horizontal θ = 4.4°±1.3° is estimated; θ = 11° is the definite upper limit.
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Abdussamatov, H. I.: 1970, Soviet Astron. A.J. 14, 64.
Abdussamatov, H. I.: 1971, Solar Phys. 16, 384.
Abdussamatov, H. I. and Krat, V. A.: 1970, Solar Phys. 14, 132.
Abetti, G.: 1957, The Sun, London, p. 157.
Beckers, J. M.: 1977, Astrophys. J. 213, 900.
Backers, J. M. and Schröter, E. H.: 1968a, Solar Phys. 4, 303.
Beckers, J. M. and Schröter, E. H.: 1968b, in K. O. Kiepenheuer (ed.), ‘Structure and Development of Solar Active Regions’, IAU Symp. 35, 178.
Beckers, J. M. and Schröter, E. H.: 1969, Solar Phys. 10, 384.
Bumba, V.: 1960, Izv. Krymsk. Astrofiz. Obs. 23, 253.
Galloway, D. J.: 1975, Solar Phys. 44, 409.
Gopasyuk, S. I.: 1977, Izv. Krymsk. Astrofiz. Obs. 57, 107.
Harvey, J.: 1971, Publ. Astron. Soc. Pacific 83, 539.
Kneer, F.: 1973, Solar Phys. 28, 361.
Maltby, P.: 1960, Ann. Astrophys. 23, 983.
Mamadazimov, M.: 1970, Soln. Dann. No. 10, 84.
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Abdussamatov, H.I. On mass flow in a complex sunspot. Sol Phys 65, 197–203 (1980). https://doi.org/10.1007/BF00151393
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DOI: https://doi.org/10.1007/BF00151393