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Satellite and ground-based observations from e.g. SOHO, TRACE, STEREO,
Hinode, SDO and IRIS to DST/ROSA, IBIS, CoMP, STT/CRISP have provided a wealth of
evidence of waves and oscillations present in a wide range of spatial scales of the
magnetised solar atmosphere. Our understanding about localised solar structures has
been considerably changed in light of these high spatial and time resolution
observations. However, MHD waves not only enable us to perform sub-resolution
magneto-seismology of magnetic waveguides but are also potential candidates to carry
and damp the necessary non-thermal energy in these localised waveguides. First, we
will briefly outline the basic recent developments in MHD wave theory focussing on
linear waves.
Next, we will concentrate on the role of the most frequently studied wave classes,
including the Alfven, and magneto-acoustic kink and sausage waves. The current
theoretical (and often difficult) interpretations of the detected solar atmospheric
wave and oscillatory phenomena within the framework of MHD will be shown. Their
photospheric origin and generation mechanism and how these waves penetrate into the
chromosphere, transition region or even into the corona will be addressed.
Last, the latest reported observational findings of potential MHD wave flux, in
terms of localised plasma heating, in the solar atmosphere with some surprising
results will be discussed, bringing us closer to solve the coronal heating problem. |
