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STP12 Abstracts Berlin, 12 - 16 July 2010 SCOSTEP Symposium 2010 Long-term variability in geomagnetic activity and storminess: Implications for solar and heliospheric structure and development Mursula Kalevi University of Oulu Geomagnetic activity forms one of the most reliable and versatile ways to study the long-term change in the Sun and heliosphere. Continuous measurements of geomagnetic activity exist since the mid-19th century, covering nearly 170 years. In addition to the long-term trend, geomagnetic activity depicts persistent patterns and periodicities, the most dominant of which are the solar cycle variation and the semiannual variation. Other significant periodicities include the annual variation, 1.3-1.8-year variation and the 22-year variation. All these variations reflect fundamental properties of the Sun and the Sun-Earth connection. Interestingly, although some of these patterns are known for nearly 150 years, they are properly appreciated and understood only since recently. In this contribution I review the present status of the traditional and new indices of geomagnetic activity, discuss the present understanding of the systematic patterns reflected in geomagnetic activity, including the centennial change of geomagnetic activity and their implications on the long-term change of the Sun.
STP12 Abstracts Berlin, 12 - 16 July 2010 SCOSTEP Symposium 2010 High-speed solar wind streams influence on relativistic electrons in the outer earth's radiation belt during the solar activity minimum. Myagkova Irina , Kalegaev Vladimir SINP MSU One of the goals of the experiment on board Russian space solar observatory CORONAS- Photon is the investigation of the space weather, in particular the relativistic electron flux dynamics in the radiation belt of the Earth’s behavior. Although, geomagnetic activity during whole 2009 was very low, sometime radiation conditions demonstrated variations typical for moderate magnetic storms. The increased (about two order) fluxes of the relativistic electron with the energy 1-4 MeV were measured after the small magnetic disturbance on 13 March 2009. This enhancement was caused by high-speed solar wind stream incoming to the Earth’s orbit. The next enhancement of the relativistic electron flux was observed on April, 9, after the next high-speed stream’s coming to the Earth. During the September, October and November 2009 the similar electron flux enhancements were observed also, but their amplitudes were significantly lower. Electron-M-Pesca is the semiconductor telescope was created for the detection of electrons with the energy 200 keV- 1 MeV, 1-4 MeV and > 4 MeV. These observations show that near-Earth’s environment is strongly caused by the solar wind during solar minimum. This work was partly supported by RFBR foundation grants 07-02-92004-ННС_а.
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scostep 2010 (stp12) - Leibniz-Institut für Atmosphärenphysik an der ...

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