Abstract
We model the formation of solar quiescent prominences by solving numerically the non-linear, time-dependent, magnetohydrodynamic equations governing the condensation of the corona. A two-dimensional geometry is used. Gravitational and magnetic fields are included, but thermal conduction is neglected. The coronal fluid is assumed to cool by radiation and to be heated by the dissipation of mechanical energy carried by shock waves. A small, isobaric perturbation of the initial thermal and mechanical equilibrium is introduced and the fluid is allowed to relax. Because the corona with the given energy sources is thermally unstable, cooling and condensation result.
When magnetic and gravitational fields are absent, condensation occurs isotropically with a strongly time-dependent growth rate, and achieves a density 18 times the initial density in 3.5 × 104 s. The rapidity of condensation is limited by hydrodynamical considerations, in contrast to the treatment of Raju (1968). When both magnetic and gravitational fields are included, the rate of condensation is inhibited and denser material falls.
We conclude that: (1) condensation of coronal material due to thermal instability is possible if thermal conduction is inhibited; (2) hydrodynamical processes determine, in large part, the rate of condensation; (3) condensation can occur on a time scale compatible with the observed times of formation of quiescent prominences.
Similar content being viewed by others
References
Allen, C. W.: 1963, Astrophysical Quantities, 2nd ed., Athlone Press, London.
d'Azambuja, L. and d'Azambuja, M.: 1948, Ann. Obs. Paris-Meudon 6, No. 7.
Brown, A.: 1958, Astrophys. J. 128, 646.
Cox, D. P. and Tucker, W. H.: 1969, Astrophys. J. 157, 1157.
Doherty, L. R. and Menzel, D. H.: 1965, Astrophys. J. 141, 251.
Field, G. B.: 1965, Astrophys. J. 142, 531.
Freeman, J. R. and Lane, F. O.: 1968, in APS Topical Conf. on Numerical Simulation of Plasma, Los Alamos Sci. Lab. Rept. LA-3990, Paper C7.
de Groot, S. R. and Mazur, P.: 1962, Non-Equilibrium Thermodynamics, North-Holland Publ. Co., Amsterdam.
Hildner, E.: 1971, Ph.D. Thesis, University of Colorado.
Hirayama, T.: 1964, Publ. Astron. Soc. Japan 16, 105.
Hunter, J. H., Jr.: 1966, Icarus 5, 321.
Hunter, J. H., Jr.: 1970, Astrophys. J. 161, 451.
Kippenhahn, R. and Schlüter, A.: 1957, Z. Astrophys. 43, 36.
Kleczek, J.: 1957, Bull. Astron. Inst. Czech. 8, 120.
Kleczek, J.: 1958, Bull. Astron. Inst. Czech. 9, 115.
Kulikovsky, A. G. and Lyubimov, G. A.: 1965, Magnetohydrodynamics, Addison-Wesley, Reading, Mass.
Kuperus, M. and Tandberg-Hanssen, E.: 1967, Solar Phys. 2, 39.
Lüst, R. and Zirin, H.: 1960, Z. Astrophys. 49, 8.
Nakagawa, Y.: 1970, Solar Phys. 12, 419.
Noyes, R. W., Dupree, A. K., Huber, M. C. E., Parkinson, W. H., Reeves, E. M., and Withbroe, G. L.: 1972, Harvard College Observatory, TR-35.
Oster, L. and Sofia, S.: 1966, Astrophys. J. 143, 944.
Parker, E. N.: 1953, Astrophys. J. 117, 431.
Piddington, J. H.: 1954a, Monthly Notices Roy. Astron. Soc. 114, 638.
Piddington, J. H.: 1954b, Monthly Notices Roy. Astron. Soc. 114, 651.
Pottasch, S. R.: 1965, Bull. Astron. Inst. Neth. 18, 7.
Raadu, M. A. and Kuperus, M.: 1973, Solar Phys. 28, 77.
Raju, P. K.: 1968: Monthly Notices Roy. Astron. Soc. 138, 479.
Richtmyer, R. D. and Morton, K. W.: 1967, Difference Methods for Initial-Value Problems, Interscience, New York.
Roberts, K. V. and Potter, D. E.: 1970, Methods Comput. Phys. 9, 339.
Tandberg-Hanssen, E.: 1967, Solar Activity, Blaisdell, Waltham, Mass.
Tandberg-Hanssen, E. and Anzer, U.: 1970, Solar Phys. 15, 158.
Uchida, Y.: 1963a, Publ. Astron. Soc. Japan 15, 65.
Uchida, Y.: 1963b, Publ. Astron. Soc. Japan 15, 376.
Weyman, R.: 1960, Astrophys. J. 132, 380.
Author information
Authors and Affiliations
Additional information
The National Center for Atmospheric Research is sponsored by the National Science Foundation.
Rights and permissions
About this article
Cite this article
Hildner, E. The formation of solar quiescent prominences by condensation. Sol Phys 35, 123–136 (1974). https://doi.org/10.1007/BF00156962
Received:
Issue Date:
DOI: https://doi.org/10.1007/BF00156962