Abstract
The results of investigation of the cyclotron wave instability in the corona for Bernstein modes and plasma waves in a hybrid band have been used to interpret zebra-pattern phenomena. Two models of the generation region of parallel drifting bands are considered: the model of the point source localized at the apex of the magnetic trap and the model of a distributed source extended along the magnetic flux tube. In the first model it is assumed that a harmonic character of zebrapattern appears either in coalescence of excited Bernstein modes at different harmonics of the gyrofrequency or in coalescence of these modes with plasma waves excited in the hybrid band. In the latter case if the magnetic field changes in time a pulsating generation regime occurs. In the second model, the emission bands appear in the regions of double plasma resonance as a result of coalescence of longitudinal waves excited in the hybrid band. Estimations of the magnetic field and the nonequilibrium component density necessary for the zebra-pattern to generate are presented.
Article PDF
Similar content being viewed by others
Avoid common mistakes on your manuscript.
References
Chiuderi, C., Giachetti, R., and Rosenberg, H.: 1973, Solar Phys. 33, 225.
Elgarøy, Ø.: 1961, Astrophysica Norvegica, 7, 123.
Rosenberg, H.: 1972, Cosmic Plasma Physics, ed. by K. Schindler, Plenum Press, New York and London, p. 191.
Slottje, C.: 1972a, Proceedings of the 2nd Meeting of the CESRA, 1971, (Trieste), p. 88.
Slottje, C.: 1972b, Solar Phys. 25, 210.
Zaitsev, V. V. and Stepanov, A. V.: 1974, Soviet Solar Data 11, 71.
Zaitsev, V. V. and Stepanov, A. V.: 1975, Astron. Astrophys., in press.
Zheleznyakov, V. V. and Zlotnik, E. Ya.: 1971, Solar Phys. 20, 85.
Zheleznyakov, V. V. and Zlotnik, E. Ya.: 1975a, Solar Phys. 43, 431.
Zheleznyakov, V. V. and Zlotnik, E. Ya.: 1975b, Solar Phys., this issue, p. 447.
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Zheleznyakov, V.V., Zlotnik, E.Y. Cyclotron wave instability in the corona and origin of solar radio emission with fine structure. Sol Phys 44, 461–470 (1975). https://doi.org/10.1007/BF00153225
Received:
Revised:
Issue Date:
DOI: https://doi.org/10.1007/BF00153225