Abstract
Distributions of brightness and polarization,p, were obtained for the February 16, 1980 solar corona. Isophotes have a circular shape, typical for the period of the solar cycle maximum. A variety of structural features are distinctly seen in the distribution ofp. The polarization reaches 55%, and thep values are comparatively high, not only in the well-defined streamers, but in the overlapping faint rays and small streamers, as well. A theoretical interpretation of the observed high degrees of polarization, taking into account the data on coronal brightness, is very difficult. This cannot be done within the scope of spherically symmetric models of the corona; the assumption of a high concentration of coronal matter into the plane of the sky is needed. With the most extreme densities in coronal structures, it is not, however, possible to exceed the observed valuep = 55%. Taking into account the accuracy of the polarization measurements, there are no reasons to reject the Thomson scattering as a basic mechanism to explain the origin of the white-light corona.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
Badalyan, O. G.: 1986,Astron. Astrophys. 169, 305.
Badalyan, O. G.: 1988,Physics of Solar Activity, Nauka, Moscow, p. 88.
Badalyan, O. G. and Livshits, M. A.: 1986,Solar Phys. 103, 385.
Clette, F., Cugnon, P., and Koeckelenbergh, A.: 1985,Solar Phys. 98, 163.
Dürst, J.: 1973,Astron. Mitt. Zürich, No. 320, 1.
Dürst, J.: 1976,Solar Phys. 50, 457.
Dürst, J.: 1982,Astron. Astrophys. 112, 241.
Koutchmy, S., and Lamy, P. L.: 1985, in R. H. Giese and P. L. Lamy (eds.),Properties and Interactions of Interplanetary Dust, p. 63.
Livshits, M. A. and Sýkora, J.: 1983,Astron. Zh. 60, 340.
Lousif, M. L.: 1987, in R. C. Altrock (ed.),9th Sacramento Peak Workshop Proc., p. 406.
Saito, K.: 1970,Ann. Tokyo Astron. Obs., Ser. 2 12, 53.
Streete, J. L. and Lacey, L. B.: 1982,Proc. Indian Nat. Sci. Acad. Suppl., Part A, No. 3, p. 81.
Sýkora, J.: 1980,Bull. Astron. Soc. India 8, 73.
Rušin, V. and Rybanský, M.: 1983a,Bull. Astron. Inst. Czech. 34, 257.
Rušin, V. and Rybanský, M.: 1983b,Bull. Astron. Inst. Czech. 34, 265.
Rušin, V. and Sýkora, J.: 1981,Bull. Astron. Inst. Czech. 32, 59.
Van de Hulst, H. C.: 1950,Bull. Astron. Inst. Neth. 11, 135.
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Badalyan, O.G., Livshits, M.A. & Sýkora, J. Polarization of the white-light corona and its large-scale structure in the period of solar cycle maximum. Sol Phys 145, 279–290 (1993). https://doi.org/10.1007/BF00690656
Received:
Revised:
Issue Date:
DOI: https://doi.org/10.1007/BF00690656