The occurrence rate of type III solar bursts in the frequency range 4.9 MHz to 30 kHz is analyzed as a function of burst intensity and burst arrival direction. We find that (a) the occurrence rate of bursts falls off with increasing flux, S, according to the power law S -1s, and (b) the distribution
The starting frequencies of type III bursts
β Scribed by J. McKim Malville
- Publisher
- Springer
- Year
- 1967
- Tongue
- English
- Weight
- 393 KB
- Volume
- 2
- Category
- Article
- ISSN
- 0038-0938
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β¦ Synopsis
During the period 1960 to 1966 the monthly averages of the starting frequencies of type II[ bursts declined with the level of solar activity and reached a minimum near the minimum of the solar cycle in 1964. The electron densities corresponding to the observed starting frequencies are close to those expected at the base of the K corona. It is shown that sufficient free-free absorption may occur in the corona above the appropriate plasma levels to account for the observed behavior of the starting frequencies of the bursts. The daily variation in the starting frequencies is attributed to structural variation of the inner corona. Quiescent prominences may be responsible for establishing periods of anomalously low-starting frequencies.
π SIMILAR VOLUMES
Solar type III bursts have been observed at fixed frequencies of 18, 22, 26 and 36 MHz during the period 1970-1974. 103 profiles have been al~alyzed in the manner introduced by Aubier and . Boischot (1972) whose results are generally confirmed. Average values for the exciter function duration were f
Observations of type III burst profiles at 18, 22, 26 and 36 MHz, by Barrow and Achong (1975), are used to calculate the form of the exciter function. The burst profile is treated as the convolution of an exciter function and an exponential decay function. The average form of the exciter profile is
Storms of type III solar radio bursts observed from 5.4 ot 0.2 MHz consist of a quasi-continuous production of type III events observable for half a solar rotation but persisting in some cases for well over a complete rotation (Fainberg and Stone, 1970). The observed burst drift rates are a function