Abstract
Profile changes of five magnetically non-split lines going from the photosphere to faculae are investigated. The observations show that the profiles normalized to the continuum differ from those of the undisturbed photosphere only in the core. The outer parts of the profiles remain unchanged. Calculations using two recent facular models do not represent these observed profile changes. It is shown that a temperature increase in outer layers h≳ 250 km does explain the observations. The problem of photospheric magnetograph calibration for facula magnetic field measurements is discussed.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
Badaljan, O. G.: 1968, Solar Data 5, 105.
Chapman, G. A. and Sheeley, N. R.: 1968, Solar Phys. 5, 442.
Grossmann-Doerth, U.: 1970, Solar Phys. 13, 287.
Harvey, J. and Livingston, W.: 1969, Solar Phys. 10, 283.
Holweger, H: 1967, Z. Astrophys. 65, 365.
Kuz'minykh, V. D.: 1963, Soviet Astron. 7, 323.
Kuz'minykh, V. D.: 1965, Soviet Astron. 8, 551.
Milkey, R. W.: 1970, Solar Phys. 14, 62.
Schmahl, G.: 1967, Z. Astrophys. 66, 81.
Stellmacher, G. and Wiehr, E.: 1970, Astron. Astrophys. 7, 432.
Unsöld, A.: 1956, Physik der Sternatmosphären, Springer, Berlin-Heidelberg.
Wiehr, E.: 1970, Solar Phys. 11, 399.
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Stellmacher, G., Wiehr, E. Magnetically non-split lines in faculae. Sol Phys 18, 220–225 (1971). https://doi.org/10.1007/BF00145934
Received:
Issue Date:
DOI: https://doi.org/10.1007/BF00145934