Abstract
This paper discusses the outflow of ions in an open magnetic field region in the solar corona. The model is polytropic and assumes that the ions do not affect the motion of the protons; treatment of large openings of the flux tubes is included.
It is found that a large variety of topologies in the velocity-heliocentric distance plane occurs, by varying the funnelling factor and the proton density. While for low proton densities the topology is characterized by a single critical point, above some value of the density and of the funnelling factor multiple critical points appear, causing the ion velocity to become large in the low corona. All the ions studied (He iii, Fe xv, Si xii, Mg x) show the same general trend, although their sensitivity to the proton density is different.
The abundance increase in the low corona, with respect to interplanetary space, is depressed if the opening of the flux tubes increases; however, for some extreme values of the acceleration due to large openings of the flux tubes, the theory predicts, on the contrary, very large increases of the coronal abundances.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
Alloucherie, Y.: 1970, J. Geophys. Res. 75, 6899.
Bame, S. J.: 1972, in C. P. Sonett, P. J. Coleman Jr., and J. M. Wilcox (eds.), Solar Wind, NASA SP-380, p. 535.
Bame, S. J., Asbridge, J. R., Feldman, W. C., Montgomery, M. D., and Kearney, P. D.: 1975, Solar Phys. 43, 463.
Bame, S. J., Asbridge, J. R., Feldman, W. C., and Gosling, J. T.: 1977, J. Geophys. Res. 82, 1487.
Borrini, G. and Noci, G.: 1978, in S. Dumont and J. Rösch (eds.), Plein Feux sur la Couronne Solaire, CNRS, Paris, p. 395.
Delache, P.: 1967, Ann. Astrophys. 30, 827.
Drago, F. C. and Poletto, G.: 1977, Astron. Astrophys. 60, 227.
Dulk, G. A., Sheridan, K. V., Smerd, S. F., and Withbroe, G. L.: 1977, Solar Phys. 52, 349.
Geiss, J., Hirt, P., and Leutwyler, H.: 1970, Solar Phys. 12, 458.
Hirshberg, J.: 1972, in C. P. Sonett, P. J. Coleman Jr., and J. M. Wilcox (eds.), Solar Wind, NASA SP-308, p. 582.
Hirshberg, J.: 1973, Rev. Geophys. Space Phys. 11, 115.
Hirshberg, J., Asbridge, J. R., and Robbins, D. E.: 1972, J. Geophys. Res. 77, 3583.
Holzer, T. E.: 1977, J. Geophys. Res. 82, 23.
Hundhausen, A. J.: 1972, Coronal Expansion and Solar Wind, Springer-Verlag, Berlin, Heidelberg, New York.
Jokipii, J. R.: 1966, in R. J. Mackin, Jr. and M. Neugebauer (eds.), The Solar Wind, Pergamon, New York, p. 215.
Joselyn, J. and Holzer, T. E.: 1978, J. Geophys. Res. 83, 1019.
Kopp, R. A. and Holzer, T. E.: 1976, Solar Phys. 49, 43.
Levine, R. H., Altschuler, M. D., and Harvey, J. W.: 1977, J. Geophys. Res. 82, 1061.
Moreno, G. and Palmiotto, F.: 1973, Solar Phys. 30, 207.
Munro, R. H. and Jackson, B. V.: 1977, Astrophys. J. 213, 874.
Nakada, M. P.: 1969, Solar Phys. 7, 302.
Nakada, M. P.: 1970, Solar Phys. 14, 457.
Neugebauer, M. and Snyder, C. W.: 1966, J. Geophys. Res. 71, 4469.
Noble, L. M. and Scarf, F. L.: 1963, Astrophys. J. 138, 1169.
Ogilvie, K. W. and Hirshberg, J.: 1974, J. Geophys. Res. 79, 4595.
Parker, E. N.: 1966, in R. J. Mackin and M. Neugebauer (eds.), The Solar Wind, Pergamon, New York, p. 23.
Robbins, D. E., Hundhausen, A. J., and Bame, S. J.: 1970, J. Geophys. Res. 75, 1178.
Yeh, T.: 1970, Planetary Space Sci. 18, 199.
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Borrini, G., Noci, G. Dynamics and abundance of ions in coronal holes. Sol Phys 64, 367–389 (1979). https://doi.org/10.1007/BF00151447
Received:
Issue Date:
DOI: https://doi.org/10.1007/BF00151447