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On the manifestation in the Sun-as-a-star magnetic field measurements of the quiet and active regions

Published online by Cambridge University Press:  26 August 2011

Mikhail Demidov
Mikhail Demidov*
Affiliation:
Institute of Solar-Terresrial Physics, P.O. Box 291, 664033 Irkutsk, Russia email: demid@iszf.irk.ru
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Abstract

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The best way to test the stellar magnetic field mapping codes is to apply them, with some changes, to the Sun, where high-precision disk-integrated and disk-resolved observations are available for a long time. Data sets of the full-disk magnetograms and the solar mean magnetic fields (SMMF) measurements are provided, for example, by the J.M.Wilcox Solar observatory (WSO) and by the Sayan Solar observatory (SSO). In the second case the measurements in the Stokes-meter mode simultaneously in many spectral lines are available. This study is devoted to analysis of the SSO quasi-simultaneous full-disk magnetograms and SMMF measurements. Changes of the SMMF signal with rotation of the surface large-scale magnetic fields are demonstrated. Besides, by deleting of selected pixels with active regions (AR) from the maps their contribution to the integrated SMMF signal is evaluated. It is shown that in some cases the role of AR can be rather significant.

Keywords

Sun: photosphereSun: magnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S273: The Physics of Sun and Star Spots , August 2010 , pp. 56 - 60
Copyright
Copyright © International Astronomical Union 2011

References

Demidov, M. L., Zhigalov, V. V., Peshcherov, V. S., & Grigoryev, V. M. 2002, Solar Phys. 209, 217.CrossRefGoogle Scholar
Donati, J.-F., Jardine, M. M., Petit, P., Morin, J., et al. 2008, ASP Conf. Ser. 384, 156.Google Scholar
Kotov, V. A., Stepanyan, N. S., & Sherbakova, Z. A. 1977, Izv. Krymsk. Astrofiz. Obs. 56, 75.Google Scholar
Petit, P., Dintrans, B., Solanki, S. K., Donati, J.-F., et al. 2008, MNRAS. 388, 80.CrossRefGoogle Scholar
Scherrer, P. H., Wilcox, J. M., & Howard, R. 1972, Solar Phys. 22, 418.CrossRefGoogle Scholar
Scherrer, P. H., Wilcox, J. M., Svalgaard, L., & Duvall, T. L., et al. 1977, Solar Phys. 54, 353.CrossRefGoogle Scholar
Sheeley, N. R., DeVore, C. R., & Boris, J. P. 1985, Solar Phys. 98, 219.CrossRefGoogle Scholar
Strassmeier, K. G. 2009, Proc. IAU Symp.N.259. 4, 363.CrossRefGoogle Scholar