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Modeling of type III bursts dynamic spectra

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Abstract

The one-dimensional process of spatially limited electron stream propagation in the solar corona is simulated. It is shown that the beam instability development results either in strong relaxation in velocity space and inhibition of spatial diffusion (high-stream density) or in velocity space relaxation decrease and simultaneous growth of spatial stream length (low-stream density). Assuming a profile of background plasma density to be exponential, dynamic spectra of type III bursts are modeled, which shows that the emission source velocity is constant, and a duration of the burst emission at a given frequency reduces for high-stream densities.

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Authors and Affiliations

  1. Institute of Solar-Terrestrial Physics SB RAS, P.O.Box 4026, Irkutsk, 664033, Russia

    V.G. Ledenev, E.A. Zverev & A.P. Starygin

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  1. V.G. Ledenev
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  2. E.A. Zverev
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  3. A.P. Starygin
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Ledenev, V., Zverev, E. & Starygin, A. Modeling of type III bursts dynamic spectra. Solar Physics 222, 299–310 (2004). https://doi.org/10.1023/B:SOLA.0000043564.73590.d6

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  • DOI: https://doi.org/10.1023/B:SOLA.0000043564.73590.d6

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