Hostname: page-component-cd9895bd7-gxg78 Total loading time: 0 Render date: 2024-12-25T16:47:32.608Z Has data issue: false hasContentIssue false
  • English
  • Français

Why the Chromosphere has Its Discrete Fine Structure

Published online by Cambridge University Press:  14 August 2015

Hermann U. Schmidt
Hermann U. Schmidt*
Affiliation:
Max-Planck-Institut für Physik und Astrophysik, München, Germany

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The fine structure in the chromosphere is probably controlled by magnetic flux concentrations which cellular convection produces in the photosphere. We will first deal with this flux concentration by the convection and its constraints. Then we will discuss the chromospheric network and its main constituent, the spicules. Following that we will look at the inside of the network, i.e. the fibrils.

Type
Part II: The Quiet Chromosphere: Disk Phenomena
Information
Symposium - International Astronomical Union , Volume 56: Chromospheric Fine Structure , 1974 , pp. 35 - 44
Copyright
Copyright © Reidel 1974 

References

Athay, R. G. and Thomas, R. N.: 1965, Astrophys. J. 123, 299.Google Scholar
Beckers, J. M.: 1972, Ann. Rev. Astron. Astrophys. 10, 73.Google Scholar
Burton, W. M., Jordan, C., Ridgeley, A., and Wilson, R.: 1974, this volume p. 89.Google Scholar
Clark, A. Jr. and Johnson, A. C.: 1967, Solar Phys. 2, 432.Google Scholar
Defouw, R. J.: 1970a, Astrophys. J. 160, 659, 161, 55.Google Scholar
Defouw, R. J.: 1970b, Solar Phys. 14, 42.Google Scholar
Frazier, E. N. and Stenflo, J. O.: 1972, Solar Phys. 27, 330.Google Scholar
Gabriel, N. H.: 1974, this volume, p. 295.CrossRefGoogle Scholar
Grossmann-Doerth, U. and von Uexküll, M.: 1971, Solar Phys. 20, 31.CrossRefGoogle Scholar
Hollweg, J. V.: 1972, Cosmic Electrodyn. 2, 423.Google Scholar
Kopp, R. A.: 1972, Solar Phys. 27, 373.Google Scholar
Kopp, R. A. and Kuperus, M.: 1968, Solar Phys. 4, 212.Google Scholar
Kuperus, M. and Athay, R. G.: 1967, Solar Phys. 3/4, 361.Google Scholar
Livshits, M. A. and Pikelner, S. B.: 1964, Astron. Zh. 41, 464.Google Scholar
Lüst, R. and Scholer, M.: 1966, Z. Naturf. 21a, 1098.Google Scholar
Meyer, F. and Schmidt, H. U.: 1968a, Z. angew. Math. Mech. 48, 218.Google Scholar
Meyer, F. and Schmidt, H. U.: 1968b, Astron. J. 73, 72.Google Scholar
Parker, E. N.: 1963, Astrophys. J. 138, 226, 552.CrossRefGoogle Scholar
Parker, E. N.: 1964, Astrophys. J. 140, 1170.Google Scholar
Peckover, R. S. and Weiss, N. O.: 1972, Comp. Phys. Commun. 4, 339.Google Scholar
Pikelner, S. B.: 1969, Astron. Zh. 46, 328.Google Scholar
Pikelner, S. B.: 1971a, Commun. Astrophys. Space Phys. 3, 33.Google Scholar
Pikelner, S. B.: 1971b, Solar Phys. 20, 286.Google Scholar
Reeves, E. M. and Parkinson, W. H.: 1972, Solar Phys. 24, 113.Google Scholar
Schlüter, A.: 1957, in van de Hulst, H. C. (ed.), ‘Radio Astronomy’, IAU Symp. 4, 356.Google Scholar
Simon, G. W.: 1967, Proc. Capri Sympos. Chromospheric Fine Structure. Google Scholar
Uchida, Y.: 1969, Publ. Astron. Soc. Japan 21, 128.Google Scholar
Weiss, N. O.: 1966, Proc. Roy. Soc. A293, 310.Google Scholar