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Solar Radio Noise Monitor

Monitors solar radio noise in the range from 20MHz to 18GHz

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  • System
  • data
  • Observed Data

    The observed data in the Solar Noise Monitor are divided into two parts. One is absolute solar flux observation; the other is low frequency spectrum observation.

    The values of absolute solar flux observation in 20 observation frequencies are displayed in graph form. Icheon station currently measures the data of absolute solar flux observation at 2.8GHz. The system used in KSWC in Jeju is an expanded and upgraded version of the Icheon system and has a much wider observation range, capable of exceeding 0.5GHz -18GHz. In addition, it uses 20 changeable observation frequencies. In this regard, the observation system of KSWC can serve in varying capacities, and can be used by the military, business and broadcasting sectors and more, all based on observation frequencies.

    The observation data for low frequency spectrum display solar spectrum in graph form. This system has certain overlapping frequencies for observation with Icheon station’s system using 30MHz -2500MHz range. However, as this system is capable of analyzing the regional impact of solar flares, and there is less interference by artificial radio waves in Jeju than Icheon, these two systems are operated to complement each other in order to analyze the impact and types of solar flares.

  • Observe absolute solar flux

    The absolute solar flux observation system displays the values of absolute solar flux in observation frequencies at various time intervals based on Solar Flux Unit (SFU). As the absolute solar flux can increase more than 1,000 times in value during solar flares, this graph is helpful to analyzes in detail exactly when the solar flares occurred on the surface of the Sun, how long they continued, and the extent of their impact on communications.

    Observe absolute solar flux Graph

  • Low Frequency Spectrum Observation

    Low frequency spectrum observation displays solar flares in the form of a spectrograph. In the event of solar flares, the spectra change into several types. Monitoring the changes can help predict the duration of solar flares and identify the frequency bands which are liable to experience radio interference.

    Low Frequency Spectrum Observation Graph