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The increase in knowledge of high energetic solar events, like flares and coronal mass ejections (CMEs), is of tremendous importance because of their impacts on the Earth´s atmosphere. Accelerated particles might affect the performance of satellites in the Earth´s orbit and moreover, endanger humans in space. Reconnection processes in the Earth´s magnetosphere cause the reorganization of the geomagnetic field effecting geomagnetic storms and enabling precipitation of particles deep into the geomagnetic field. In the wake of the large solar flares in October and November 2003, electric currents were induced in European and American power grids due to fluctuations in the Earth´s magnetic field which in Europe even caused power outages. Thus, a successful forecasting of these large disturbances which demands much better knowledge of their causing/driving processes, would decrease the risk of dangers. In order to address the topic of CME initiation, energy release in solar flares, and the flare-CME connection properly, we will study eruptive processes observed on different spatial scales over a broad wavelength range from X-rays to radio. The analyses will be performed collectively on ground- as well as space-based observations. We will address observational as well as theoretical aspects of the CME-flare relationship.
Short description of the task performed by Croatian partner
We will act on the hypothesis that large flares are a consequence of eruptions that provide through the feed-back relationship a prolonged CME acceleration by sustaining the electric current of the erupting magnetic torus. As a consequence the action of the Lorentz force extends to larger distances, launching the eruption into interplanetary (IP) space, i.e. causes an IP CME. There are three main goals to be achieved: a) gain better knowledge of the relative kinematics of the CME three-part structure (frontal rim, cavity, prominence) in order to address the basic question: is the magnetic arcade eruption either a consequence of loss of stability of the overall structure or is it driven by an instability of some of its parts (e.g., kink instability of highly twisted prominence in the arcade core, or the buoyant instability of the cavity); b) give details on the flare energy release; c) examine the role of reconnection in the flare to the CME acceleration.
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