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Small-Scale Magnetic Features Observed in the Photosphere

Published online by Cambridge University Press:  08 February 2017

Sara F. Martin
Sara F. Martin*
Affiliation:
Big Bear Solar Observatory Solar Astronomy 264-33 California Institute of Technology Pasadena, CA 91214, U.S.A.

Abstract

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Small-scale solar features identifiable on the quiet sun in magnetograms of the line-of-sight component consist of network, intranetwork, ephemeral region magnetic fields, and the elementary bipoles of ephemeral active regions. Network fields are frequently observed to split into smaller fragments and equally often, small fragments are observed to merge or coalesce into larger clumps; this splitting and merging is generally confined to the borders and vertices of the convection cells known as supergranules. Intranetwork magnetic fields originate near the centers of the supergranule convection cells and appear to increase in magnetic flux as they flow in approximate radial patterns towards the boundaries of the cells.

Type
III. Small-Scale Magnetic Fields
Information
Symposium - International Astronomical Union , Volume 138: Solar Photosphere: Structure, Convection and Magnetic Fields , 1990 , pp. 129 - 146
Copyright
Copyright © Kluwer 1990 

References

Chou, D. and Wang, H.: 1987, Solar Phys. 110, 81.CrossRefGoogle Scholar
Frazier, E.N.: 1972, Solar Phys. 26, 130.Google Scholar
Giovanelli, R.G.: 1982, Solar Phys. 77, 27.CrossRefGoogle Scholar
Harvey, K.L.: 1989, in preparation.Google Scholar
Harvey, K.L. and Martin, S.F.: 1973, Solar Phys. 32, 389.CrossRefGoogle Scholar
Harvey, K.L., Harvey, J.W. and Martin, S.F.: 1975, Solar Physics 40, 87.Google Scholar
Livi, S.H.B., Wang, J. and Martin, S.F.: 1985, Australian J. Phys. 38, 855.CrossRefGoogle Scholar
Martin, S.F. 1988, Solar Phys. 117, 243.Google Scholar
Martin, S.F. and Harvey, K.L.: 1979, Solar Phys. 64, 93.Google Scholar
Martin, S.F. Livi, S.H.B. and Wang, J.: 1985, Australian J. Phys. 38, 929.Google Scholar
Priest, E.R. and Forbes, T.G.: 1986, J. Geophys. Res. 91, 5579.Google Scholar
Stenflo, J.O.: 1989, Astron. Astrophys. Review 1, 3.Google Scholar
Tang, F., Howard, R.F. and Adkins, J. M.: 1984, Solar Phys. 91, 76.CrossRefGoogle Scholar
Vrabec, D.: 1974, in Athay, R.G. (ed), ‘Chromospheric Fine Structure’ , IAU Symp. 56, 201.Google Scholar
Wang, J., Shi, Z., Liu, J. Han, Feng and Liu, G.: 1989, presented at IAU Symp. 138, Kiev, 14-19 May 1989.Google Scholar
Wang, J., Shi, Z., Martin, S.F. and Livi, S.H.B.: 1988, Vistas in Astronomy , 31, 79.CrossRefGoogle Scholar
Zirin, H.: 1987, Solar Phys. 110, 101.CrossRefGoogle Scholar
Zwaan, C.: 1978, Solar Phys. 60, 213.Google Scholar
Zwaan, C.: 1985, Solar Phys. 100, 397.Google Scholar
Zwaan, C.: 1985, in Muller, R., Lecture Notes in Physics , Vol. 233, Springer-Verlag, Berlin, p.263.Google Scholar
Zwaan, C.: 1987, Ann. Rev. Astron. Astrophys. 25, 83.CrossRefGoogle Scholar