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STP12 Abstracts Berlin, 12 - 16 July 2010 SCOSTEP Symposium 2010 Theoretical and numerical modelling of solar eruptions Török Tibor LESIA, Observatoire de Paris Large-scale solar eruptions are the most violent energy release processes in the solar system and the main driver of Space Weather disturbances. They are observed as flares, CMEs, and filament (or prominence) eruptions. It is now widely accepted that these three phenomena are not independent, but constitute different observational manifestations of a more global process, namely a sudden large-scale disruption of the coronal magnetic field. While a "standard model" for the main ( flare) phase of such eruptions is now well established (often referred to as CSHKP Model), the mechanisms which trigger and drive eruptions in the first place are still not fully understood. In this talk, I will review current theoretical models for the initiation and acceleration of solar eruptions, with emphasis on the considerable progress obtained by numerical MHD simulations in recent years. In particular, I will discuss to what extent the models overlap, and briefly outline how they might converge in the coming years to a "standard model" for the initiation and acceleration of solar eruptions.
STP12 Abstracts Berlin, 12 - 16 July 2010 SCOSTEP Symposium 2010 Evolution of 3D solar wind structure during cycles 22 and 23 Tokumaru Munetoshi , Fujiki Ken'ichi , Msasyoshi Kojima Solar-Terrestrial Environment Laboratory, Nagoya University Interplanetary scintillation (IPS) measurements made with the 327-MHz multi-station system of the Solar-Terrestrial Environment Laboratory of Nagoya University were analyzed to study long-term variation of the global solar wind structure during cycles 22 and 23 (1985-2008). In this analysis, the computer-assisted tomography method was applied to retrieve threedimensional distribution of the solar wind speed from IPS observations. The result clearly demonstrated that the solar wind structure evolved drastically with the solar cycle; the source surface areas of fast (slow) wind increased systematically as the solar activity declines, reaching the maximum (minimum) value at the minimum phase. In addition, the spatial distribution of fast and slow winds showed different latitude preference. High latitude regions were mostly dominated by the fast wind except for a few years around the maximum phase, while low latitude regions were occupied with the slow wind throughout the cycle. These behaviors of fast/slow winds are regarded as manifestation of the solar cycle change of Sun's magnetic field. An excellent correlation between fast/slow wind areas and polar magnetic field is demonstrated here. The important point to note is that the solar wind speed distribution for the current minimum significantly differs from that for the previous minimum. This difference is considered as a consequence of weaker polar fields in the current minimum, and may be a part of secular variation of the solar activity.
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scostep 2010 (stp12) - Leibniz-Institut für Atmosphärenphysik an der ...

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