Abstract
In the dynamical model of quiescent prominences presented in this paper, it is assumed that the ever-changing velocity field and brightness of the fine structure is due to MHD turbulence driven by an Alfvén-wave flux from below. It is shown that these waves become highly non-linear and are dissipated over relatively short scales in prominence matter. For magnetic field strengths lower than those observed in quiescent prominences, no closed arch structure can exist with the physical parameters observed. For higher field strengths the conditions for the creation of turbulence are not fulfilled.
The momentum gained by prominence matter in the dissipation process, is shown to be of the right order of magnitude to provide the supporting force against gravity.
‘Edge’ effects find a simple explanation within the framework of this hypothesis.
In the upper regions of a prominence one result of the dissipation may be the formation of open magnetic configurations, in keeping with the presence of streamers connected with quiescent prominences. Observational tests are proposed and discussed.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
Chapman, R. D.: 1981, Solar Phys. 71, 151.
Engvold, O.: 1972, Solar Phys. 23, 346.
Engvold, O.: 1976, Solar Phys. 49, 283.
Engvold, O.: 1981, Solar Phys. 70, 315.
Engvold, O. and Leroy, J. L.: 1979, IAU Colloq. 44, 97.
Engvold, O. and Livingston, W.: 1971, Solar Phys. 20, 375.
Engvold, O., Malville, J. M., and Livingston, W.: 1978, Solar Phys. 60, 57.
Harvey, J. W.: 1969, Ph.D. thesis, Univ. of Colorado.
Harvey, J. W.: 1983, private communication.
Heyvaerts, J. and Priest, E. R.: 1983, Astron. Astrophys. 117, 220.
Hirayama, T.: 1971, Solar Phys. 19, 384.
Hollweg, J. V.: 1978, Rev. Geophys. Space Phys. 16, 689.
Hollweg, J. V., Jackson, S., and Galloway, D.: 1982, Solar Phys. 75, 35.
Jensen, E.: 1982, Solar Phys. 77, 109.
Kleczek, J.: 1980, Hvar Obs. Bull. 4, 35.
Leer, E. and Holzer, T. E.: 1980, J. Geophys. Res. 85, 4681.
Leroy, J. L., Bommier, V., and Sahal-Brechot, S.: 1983, Solar Phys. 83, 135.
Maltby, P.: 1976, Solar Phys. 46, 149.
Malville, J. M.: 1968, Solar Phys. 4, 323.
Malville, J. M. and Harvey, J. W.: 1979, IAU Colloq. 44, 77.
Martres, M. J., Mein, P., Schmieder, B., and Soru-Escaut, I.: 1981, Solar Phys. 69, 301.
Nikolsky, G. M., Gulyaev, R. A., and Nikolskaya, K. I.: 1971, Solar Phys. 21, 332.
O En Den, Kim, I. S., and Nikolsky, G. M.: 1977, Solar Phys. 52, 35.
Plocieniak, S. and Rompolt, B.: 1973, Solar Phys. 29, 399.
Saito, K. and Tandberg-Hanssen, E.: 1973, Solar Phys. 31, 105.
Severny, A. B. and Khokhlova, V. L.: 1953, Izv. Kryms. Astrofiz. Obs. 10, 9.
Smartt, R. N.: 1983, private communication.
Sýkora, J.: 1968, Bull. Astron. Inst. Czech. 19, 37.
Tandberg-Hanssen, E.: 1974, Solar Prominences, D. Reidel Publ. Co., Dordrecht, Holland.
Tandberg-Hanssen, E. and Anzer, U.: 1970, Solar Phys. 15, 158.
Tsubaki, T.: 1975, Solar Phys. 43, 147.
Waldmeier, M.: 1963, in J. W. Evans (ed.), ‘The Solar Corona’, IAU Symp. 16, 129.
Waldmeier, M.: 1970, Solar Phys. 15, 167.
Wentzel, D. G.: 1977, Solar Phys. 52, 163.
Zirker, J. B. (ed.): 1977, Coronal Holes and High Speed Wind Streams, Colorado Associated University Press.
Author information
Authors and Affiliations
Additional information
Visiting Astronomer on leave from Institute of Theoretical Astrophysics, University of Oslo, Norway.
Operated by the Association of Universities for Research in Astronomy, Inc., under contract with the National Science Foundation.
Rights and permissions
About this article
Cite this article
Jensen, E. Alfvén waves and turbulence in quiescent prominences. Sol Phys 89, 275–285 (1983). https://doi.org/10.1007/BF00217251
Received:
Issue Date:
DOI: https://doi.org/10.1007/BF00217251