How to Analyse the Data

Joachim Köppen DF3GJ Kiel/Strasbourg/Illkirch Summer 2004

Schematic dynamic spectra of the various types of solar radio bursts. Type II and III burst are relatively narrow-band and sweep from high frequency to low frequencies, rapidly or more slowly; Type IV and V are more broadband, resembling even more a broadband noise.

In a different orientation, such a spectrum is shown below, as observed with the Spectrograph at the University of Florida's Radio Observatory, built by Richard Flagg. The observations are from March 31, 2004, and more data can be found in the Radio Jove Data Archive.

One notes as horizontal red lines the strong emissions by the 13 m broadcast band near 21.6 MHz, also some strong signal around 27 MHz (CB radio) and other terestial emissions. The solar bursts are weaker (light blue), and show up as almost vertical structures, sweeping rapidly from high frequencies down. At a single frequency, such as 20 MHz, the amplitude of the two strong bursts would resemble the 'shark's fin' shape of rapid rise - slow fall. Below is a similar view, in yet another orientation, from the Nançay Decametric Array

So what we can do with our single-frequency data:

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