Volume 25 Issue 5
Sep.  2005
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V. Maksimov, D. Prosovetsky. Structure of the Program of Short-term Prediction of Powerful Solar Flares[J]. Journal of Space Science, 2005, 25(5): 329-332. doi: 10.11728/cjss2005.05.329
Citation: V. Maksimov, D. Prosovetsky. Structure of the Program of Short-term Prediction of Powerful Solar Flares[J]. Journal of Space Science, 2005, 25(5): 329-332. doi: 10.11728/cjss2005.05.329

Structure of the Program of Short-term Prediction of Powerful Solar Flares

doi: 10.11728/cjss2005.05.329
  • Received Date: 1900-01-01
  • Rev Recd Date: 1900-01-01
  • Publish Date: 2005-09-15
  • Input data of the system are two-dimensional images and one-dimensional distributions of total and polarized solar emission at 5.2 cm wavelength obtained with SSRT. Together with photoheliograms, magnetograms, Hα-filtergrams and characteristics of active regions received from other sources, they form the initial database. The first stage includes superimposing the images, identifying microwave sources with active regions, assigning NOAA numbers to the sources, and determining for each active region the heliolatitude, extent, and inclination angle of the group's axis to the equator. These data are used to calculate the boundaries of longitude zones for each active region. A next stage involves determining the brightness temperatures of microwave sources less than the polarization distribution, the degree of polarization, and microwave emission flux, as well as calculating the parameters of microwave sources. Each parameter is assigned its own value of the weight factor, and the sum of values is used to draw the conclusion about the flare occurrence probability in each active region and on the Sun in general.

     

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