The proposed STEREO/WAVES (SWAVES) instrument provides unique and critical observations for all primary science objectives of the STEREO mission.
SWAVES can probe a CME from lift-off to Earth by: - detecting the coronal and interplanetary (IP) shock of CMEs,
- providing a radial profile of CMEs through spectral imaging,
- determining the radial velocity from ~2 RS (from center of the Sun) to Earth,
- measuring the density of the volume of the heliosphere between the Sun and Earth, and
- measuring important in-situ properties of the IP shock, magnetic cloud, and density compression in the fast solar wind stream that follows.
SWAVES will achieve these goals by measuring interplanetary type II and type III radio bursts, both remotely and in-situ.
The STEREO theoretical investigations performed at IWF are addressed to dynamical and energetic processes in solar coronal magnetic loops. Two groups of models have been proposed. One group of models, so-called inductive models of loops, is addressed to the global dynamics of coronal magnetic loops, their rising, oscillations, and reconfigurations. Another group, the non-adiabatic MHD models, describes the internal dynamics of plasma in a magnetic tube.
The developed models can be applied for - explanation of the energetic processes in groups of closely located magnetic loops,
- description of acceleration of CMEs,
- description of particles acceleration during different stages of a CME formation and propagation,
- interpretation of flaring processes, formation and evolution of sources of flaring emission,
- description of the Loop-loop flaring interaction, and
- explanation of oscillations of the loops.
Theoretical studies carried out at IWF Graz are combined with the STEREO mission extensive ground-based observations and interpretation of the solar activity phenomena. These investigations are performed in close collaboration with colleagues from the world largest decameter radio telescope UTR-2 in Kharkov (Ukraine). Recent observations performed at 12 MHz allowed new types and peculiarities of the solar sporadic radio emission, such as fine time- and frequency-structures, as well as to perform more detailed studies of phenomena already known, like type III and type II bursts, drift pairs, etc.
Future observations, which are supposed to be carried out with a spectrum analyzer of a new generation, will give us an opportunity to investigate the solar activity phenomena as well as the weakly active Sun and quiet corona at the heights 0.5-1.5 R, which can be studied by other methods.
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