Abstract
Network magnetic fields, ephemeral active regions, and intranetwork magnetic fields are illustrated and discussed in several contexts. First, they are presented in relation to the appearance and disappearance of magnetic flux. Second, their properties in common with all solar magnetic features are discussed. Third, their distinguishing characteristics are emphasized. Lastly, their interactions are illustrated.
Network magnetic fields are no longer considered to be just the aged remnants of active regions. The network is the dynamic product of the merging and cancelling of intranetwork fields, ephemeral regions, and the remnants of active regions. Intranetwork fields are magnetic fields of mixed polarity that appear to originate continuously from localized source sites in between the network. The intranetwork magnetic fields are characterized by flow of successive fragments in approximately radial patterns away from their apparent source sites and by the relative weakness of their magnetic fields. Ephemeral active regions are small, new bipoles that grow as a unit or a succession of bipolar units and whose poles move in opposite directions from their apparent site of origin. Large ephemeral regions are not distinguishable from small active regions.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
Brants, J. J. and Steenbeek, J. C. M.: 1985, Solar Phys. 96, 229.
Gaizauskas, V., Harvey, K. L., Harvey, J. W., and Zwaan, C.: 1983, Astrophys. J. 265, 1056.
Harvey, K. L. and Martin, S. F.: 1973, Solar Phys. 32, 389.
Harvey, J. W., Harvey, K. L., and Martin, S. F.: 1975, Solar Phys. 40, 87.
Hermans, L. M. and Martin, S. F.: 1986, Coronal and Prominence Plasmas, NASA Publication CP 2442, p. 369.
Komle, N.: 1979, Solar Phys. 64, 213.
LaBonte, B. and Howard, R. F.: 1981, Solar Phys. 74, 131.
Livi, S. H. B., Martin, S. F., and Wang, J.: 1985, Australian J. Phys. 38, 855.
Martin, S. F.: 1984, in S. L. Keil (ed.), Small-Scale Dynamical Processes in Quiet Stellar Atmospheres, National Solar Observatory/Sacramento Peak, Sunspot, New Mexico, U.S.A., p. 30.
Martin, S. F.: 1986, Coronal and Prominence Plasmas, NASA Publication 2442, p. 73.
Martin, S. F. and Harvey, K. L.: 1979, Solar Phys. 64, 93.
Martin, S. F., Livi, S. H. B., and Wang, J.: 1985, Australian J. Phys. 38, 929.
Martin, S. F., Livi, S. H. B., Wang, J., and Shi, Z.: 1985, Proceedings of the Workshop on Vector Magnetic Fields, 18–18 May, 1984, Marshall Space Flight Center, Huntsville, Alabama, U.S.A., p. 403.
Mosher, J. M.: 1977, Ph.D. Thesis, California Institute of Technology.
Schoolman, S. A.: 1973, Solar Phys. 32, 379.
Smithson, R. C.: 1973, Solar Phys. 29, 365.
Topka, K. and Tarbell, T.: in S. L. Keil (ed.), Small-Scale Dynamical Processes in Quiet Stellar Atmospheres, National Solar Observatory, Sunspot, New Mexico, U.S.A., p. 278.
Vrabec, D.: 1971, in R. Howard (ed.), ‘Solar Magnetic Fields’, IAU Symp. 43, 329.
Vrabec, D.: 1974, in R. G. Athay (ed.), ‘Chromospheric Fine Structure’, IAU Symp. 56, 201.
Wilson, P. R. and Simon, G.: 1983, Astrophys. J. 273, 805.
Zirin, H.: 1985, Australian J. Phys. 38, 961.
Zirin, H.: 1987, Solar Phys. 110, 101.
Zwaan, C.: 1978, Solar Phys. 60, 213.
Zwaan, C.: 1985, in R. Muller, Lecture Notes in Physics, Vol. 233, Springer-Verlag, Berlin, p. 263.
Zwaan, C.: 1987, Ann. Rev. Astron. Astrophys. 25, 83.
Zwaan, C., Brants, J. J., and Cram, L. E.: 1985, Solar Phys. 95, 3.
Author information
Authors and Affiliations
Additional information
Solar Cycle Workshop Paper.
Rights and permissions
About this article
Cite this article
Martin, S.F. The identification and interaction of network, intranetwork, and ephemeral-region magnetic fields. Sol Phys 117, 243–259 (1988). https://doi.org/10.1007/BF00147246
Received:
Issue Date:
DOI: https://doi.org/10.1007/BF00147246