High-Frequency Evolving Emission Lines for the 25 August 1999 Solar Flare

Details High-Frequency Evolving Emission Lines for the 25 August 1999 Solar Flare High-Frequency Evolving Emission Lines for the 25 August 1999 Solar Flare

Jul 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008soph..250..107n&link_type=abstract

Solar Physics, Volume 250, Issue 1, pp.107-113

Physics

Flares, Radio Radiation

Scientific paper

We analyze a special kind of temporal fine structure in microwave radio emission for the 25 August 1999 solar flare observed by the PMO spectrometer over the range of 4.5 - 7.5 GHz. This flare displays continuum emission after a group of reverse-slope type III bursts around 6 GHz. High-resolution dynamic spectra reveal three evolving emission lines (EELs) following the type III group. They are characterized by isolated, narrow, and continuous emission strips, which display frequency fluctuations with time. Their frequency-drift rates are between -2 and 3 GHz s-1. Distinct from the EELs at lower frequencies, three EELs have a very short duration of a few seconds. They show an average bandwidth of Δ f≈330 MHz and a relative bandwidth of Δ f/ f≈0.057. This is the first time that this kind of fine structure has been observed around 6 GHz.

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