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Atomic Orientation in Chromospheric Lines
Published online by Cambridge University Press: 12 April 2016
Abstract
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Observations of the Stokes I and V profiles of the Ca II H and K lines in solar magnetic regions are presented. Least-squares fits of dI/dλ to V are obtained and the wavelength variation of the residuals, i. e. V-kdI/dλ, calculated. We find significant symmetric residuals in umbrae, which are in agreement with the effect on the V profiles due to atomic orientation, i.e. with the existence of an unequal population of the Zeeman sublevels with M>0 with respect to those with M<0.
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- Session 9. Convections and Oscillation in Active Regions
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- Copyright © Astronomical Society of the Pacific 1993
References
Laudi Degl’Innocenti, E., 1985, in Theoretical Problems in High Resolution Solar Physics ed. Schmidt, H.U., MPA
212, p.162
Google Scholar
Martínez Pillet, V., García, López, del Toro Iniesta, J.C., Rebolo, R., Vázquez, M., Beckman, J., Char, S., 1990, Ap.J., 361, L81
Google Scholar
Sánchez Almeida, J., Martínez Pillet, V., 1990, in Advancesin Solar Polarimetry, ed. November, L., NSO/SP SW
11, p. 191
Google Scholar
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