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STP12 Abstracts Berlin, 12 - 16 July 2010 SCOSTEP Symposium 2010 Outer radiation belt of relativistic electrons in 2006-2010: GLONASS data Tverskaya Liudmila 1 , Balashov Sergey 2 , Ivanov Vladimir 2 , Karpenko Dmitry 2 , Kochura Sergey 2 , Maximov Igor 2 , Pavlov Nikolay 1 , Reizman Svetlana 1 , Rubinstein Iliya 1 , Sitnikova Ninel 2 , Teltsov Michael 1 , Trofimchuk Denis 2 , Tulupov Vladimir 1 , Vedenkin Nikolay 1 1 Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow, 119991, Russia, 2 The Joint-stock Company ”Academician M.F. Reshetnev” Information Satellite Systems”, 52, Lenin Str., Zheleznogorsk, Krasnoyarsk region, 662972, Russia We analyze a dataset of 1 MeV electrons measured on GLONASS in 2006-2010. Radiation doze under 2 g/cm 2 Al is also presented. The orbit is circular, 20000 km height, 65 degrees inclination; it well covers the outer radiation belt. Semiannual-mean doze shows unprecedented decrease by ~20 times, from 2007 to 2009. This gives more than order of magnitude deviation from the model-based (AE8) prediction. Generally, fluxes of relativistic electrons become lower and lower along these years, with yet rather high individual peaks. Seldom and weakening storms leave quiescent periods in which diffusion waves of earthward moving belts of newly injected electrons can be easily observed. Wave velocity well corresponds to the theory of L-diffusion of electrons driven by sudden geomagnetic impulses. Seasonal variation (with maxima around equinoxes) is seen but not in all periods and not so well as we saw on GLONASS in 1994-1996. A most prominent breaking of the seasonal cycle is a high-amplitude peak in Dec 2006, resulted from injection by the strong geomagnetic storm; this storm also breaks seasonal variation of geomagnetic indices.
STP12 Abstracts Berlin, 12 - 16 July 2010 SCOSTEP Symposium 2010 CHAIN Project and Capacity Building Ueno Satoru 1 , Shibata Kazunari, Ichimoto Kiyoshi, Kitai Reizaburo, Nagata Shin'ichi, Kimura Goichi, Nakatani Yoshikazu, Morita Satoshi 1 Kwasan and Hida Observatories, Kyoto University, 2 The Flare Monitoring Telescope (FMT) was constructed in 1992 at Hida observatory in Japan to investigate the long-term variation of solar activity and explosive events. It has been part of the international coordinated observations program (STEP) since 1991. It has five solar imaging telescopes that SIMULTANEOUSLY observe the full-disk Sun at different wavelengths around H-alpha absorption line or in different modes. Therefore, it can measure the 3 dimensional velocity field of gas motion of active phenomena on the full solar disk with suppressing the seeing effect. Moreover, it can detect Moreton-waves (shockwaves on the chromosphere) that accompany solar flares. Observations of physical properties of such solar explosive phenomena play a very important role for the space-weather research. We want to monitor all geoeffective solar flares, erupting filaments and shock waves as much as possible by using several of such characteristic telescopes. Then, we started to execute "Continuous H-alpha Imaging Network (CHAIN)-project" as part of the CAWSES, CAWSES-II project. In the CHAIN-project, we intend to install the FMT-type telescopes in foreign appropriate sites, so that we achieve 24 hr continuous observational network. As for the station for the 1 st oversea FMT, we selected Ica University in Peru and we already installed it there in March 2010 with cooperation of Peru/IGP* and Ica Univ. Moreover, we are planning to install the 2 nd oversea FMT to Algeria in around 2012 with cooperation of Algeria/CRAAG**. Through such distributions of instruments under the CHAIN-project, we aim to advance international cooperative studies, education and popularization of space weather research and solar physics. These are also important purposes of the CHAIN-project. Therefore, this project is quite fit for not only the scientific purpose of CAWSES-II, but also the purpose of capacity building. In this talk, we would like to introduce characteristics of the CHAIN-project, current status and plans in the next several years. (*) IGP: Instituto Geofisico del Peru (**) CRAAG: Centre de Recherche en Astronomie Astrophysique et Geophysique
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scostep 2010 (stp12) - Leibniz-Institut für Atmosphärenphysik an der ...

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