Abstract
THE most prominent feature of solar bursts of spectral type III is their frequency drift from higher to lower frequencies. Wild1 has determined the drift velocity in the frequency region of 70–130 Mc/s, but until now there have been no satisfactory determinations of the drift rate on higher frequencies.
Similar content being viewed by others
Article PDF
References
Wild, J. P., Austral. J. Sci. Res., A, 3 (1950).
Newkirk, G., Astrophys. J., 133, 3 (1961).
de Jager, C., Handb. Phys., 52 (1959).
Weiss, A. A., and Sheridan, K. V., J. Phys. Soc. (Japan), 17, A, 2 (1962).
Hepburn, N., Astrophys. J., 122 (1955).
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
ELGARØY, Ø., RØDBERG, H. Frequency Drift and Time Profile of 200 Mc/s Bursts of Type III and the Electron Temperature of the Corona. Nature 199, 268 (1963). https://doi.org/10.1038/199268a0
Issue Date:
DOI: https://doi.org/10.1038/199268a0
This article is cited by
-
Observations of beam propagation
Solar Physics (1990)
-
Type III solar radio burst storms observed at low frequencies
Solar Physics (1970)
-
Type III radio bursts in the outer corona
Solar Physics (1969)
Comments
By submitting a comment you agree to abide by our Terms and Community Guidelines. If you find something abusive or that does not comply with our terms or guidelines please flag it as inappropriate.