Magnetohydrodynamic Wave Diagnostics of the Solar .. (SeismoSun)
Magnetohydrodynamic Wave Diagnostics of the Solar Atmosphere in the Era of Transformative High-Resolution Observations
Date du début: 1 avr. 2013,
Date de fin: 31 mars 2018
Funding is sought for a 5-year project supporting two postdoctoral research assistants and two 4-year PhD studentships to carry out a research programme on qualitative advances of our understanding of basic physical processes operating in the atmosphere of the Sun. This will be accomplished by the use of the unprecedented high-resolution data obtained with the new generation of solar space missions, which allow us to fully implement the novel technique for plasma diagnostics, based upon magnetohydrodynamic waves. The project aims to reveal the mechanisms behind the most intriguing and disturbing solar phenomena: the heating of the corona and the physics of solar flares and mass ejections. The specific objectives are to develop and apply innovative techniques for determining the plasma’s heating function and the characteristic spatial scale of fine structuring; the method for instant diagnostics of plasma parameters by propagating wave trains; the technique for the determination of microphysical processes by macroscopic observables; to discriminate observationally between the theoretically predicted regimes of powerful releases of magnetic energy; to create a theoretical and observational foundation for stellar coronal seismology; and to implement novel methods for the analysis of wave phenomena in spatially-resolved observational data. The project is based upon the synthesis of analytical and numerical theoretical studies and forward modelling of observables, accounting for both magnetohydrodynamic and kinetic effects, and the analysis of multi-wavelength data obtained with space missions SDO, Hinode and STEREO and the Nobeyama radioheliograph. The knowledge to be gained from the project – robust and detailed diagnostics of key parameters and fundamental processes operating in the solar atmosphere – is of vital importance for the creation of models with a predictive value, and for further progression of solar, space and astro plasma physics.
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