Seismology of the solar corona with slow magnetoacoustic waves

Modern spaceborne EUV imagers provide us with the confident detection of various kinds of magnetohydrodynamic (MHD) waves in plasma non-uniformities of the corona of the Sun. In particular, slow magnetoacoustic waves are manifested as propagating or standing field-aligned disturbances of the intensity of EUV emission or Doppler shifts of coronal emission lines, with typical observed or estimated speeds about the estimated sound speed. The aim of the project is to develop and apply novel methods of the seismological estimation of coronal heating function and/or transport coefficients and fine plasma structuring by the slow waves. In the project, the student will perform comprehensive analysis of propagating slow waves observed in plasma fan-like structures of coronal active regions and in plume structures in coronal holes. The attention will be paid to long-term variability of the wave parameters, such as instantaneous oscillation periods, apparent speeds and amplitudes, and their correlations with each other and parameters of waveguiding plasma non-uniformities. The required high-precision observational data will be obtained from the SDO/AIA and SolO/EUI archives. The data analysis will be supplemented by theoretical modelling in terms of MHD wave theory, accounting for the effect of wave-induced thermal misbalance.