Abstract
The distribution of oscillation-amplitude for Doppler shifts in chromospheric lines is computed as a function of position on the disk and time frequency. High amplitude regions are restricted to a small part of the solar surface. Propagation modes are investigated with respect to the oscillation amplitude in the K line. Waves seem to be standing or evanescent for most of the points (small amplitude in K) and progressive for some other ones, with perhaps upward and downward motions (partial reflections). Mechanical energy could only escape into corona from narrow chromospheric structures.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
Cram, L. E., Brown, D. R., and Beckers, J. M.: 1977, Astron. Astrophys. 51, 211.
Deuber, F. L.: 1972, Solar Phys. 22, 263.
Dumont, S.: 1967, Ann. Astrophys. 30, 421.
Edmonds, F. N.: 1966, Astrophys. J. 144, 733.
Mein, N.: 1977, Solar Phys. 52, 283.
Mein, N. and Mein, P.: 1976, Solar Phys. 49, 231.
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Mein, N. Relation between the mode of oscillation and the velocity amplitude of chromospheric waves. Sol Phys 59, 3–9 (1978). https://doi.org/10.1007/BF00154926
Received:
Revised:
Issue Date:
DOI: https://doi.org/10.1007/BF00154926