Solar Extreme Events of 2003:
Fundamental Science and Applied Aspects

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Special features of sporadic solar radio emission during 2-hour interval of CMEs formation and initial propagation (according to the data of the world service of the solar radio emission in 2003)
Durasova M.S., Tikhomirov Yu.V., Fridman V.M., Sheiner O.A.,

The comparison of observational data in 2003 (the CMEs parameters recorded by LASCO and the characteristics of sporadic solar radio emission, undertaken from the worldwide network of data of the service of the Sun in the radio-frequency band) is carried out. Data cover the twenty-four hour measurements of the solar fluxes and their variations. At the same time the spectral working range of 410 - 15400 MHz is not complete for the 24-hour period. They are undertaken as the basic CMEs parameters: CMEs' phenomenological type, velocity of CMEs propagation, angular width and the central meridian of the recorded event. They are examined as the characteristics of sporadic solar radio emission being investigated: duration and intensity of phenomena in cm and dm wavelength ranges, and the phenomenological type of those recorded bursts according to international classification accepted, as well. So called isolated CMEs events are selected for a study. It is the situation when during the 8-hour time interval before and 6-hour time interval after these CMEs there were no other recorded CMEs events. This makes it possible to consider the observed sporadic component of radio emission as associated with the event in question. The connections between the CMEs parameters and the characteristics of the sporadic radio emission are established. There is the absence of sporadic phenomena in cm the wavelength range in the majority of the high-speed (velocity more than 500 km/s) and strongly directed (the angular width of event about 50 degrees) CMEs events. The special features of sporadic radio emission before the CMEs events, projected to the region of the north pole of the Sun are observed. The model presentations, which make it possible to confirm the results indicated, are discussed. The work is fulfilled with the support of Russian Foudation for Basic Research (grant 03-02-16691), Ministry of Science and Education (grant E02-11.0-27), and FPSTP (Astronomy) and FPP (Space Weather).





Skobeltsyn Institute of Nuclear Physics, Moscow State University, 2004