The Lustbühel Radio Station is devoted to study the magnetized plasma of the solar system. A crossed log-periodic antenna is used to collect the radio emission coming from the outer part of the solar atmosphere, i.e. solar corona, in the frequency range from 30 MHz to 150 MHz. Regularly, the Sun is observed two hours before and after the local meridian. The antenna is connected to a digital spectropolarimeter (DSP) receiver which has a frequency bandwidth of 12.5 MHz and a spectral resolution of 1 ms and
<nobr>12.5 kHz</nobr>, respectively. The receiver provides a dynamic spectrum which represents the variation of the solar radio emission versus time and frequency. These emissions are associated with solar radio bursts generated by electron beams propagating along open magnetic field lines, e.g. type III as shown in the figure.
IWF investigates in particular the fine structures, like drift-pairs, observed during solar radio flares. The ground-based observations are combined with WAVES experiment observations on board of the WIND satellite.
Further information on WIND can be found at NASA.
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