Solar Magneto-Seismology: A Novel Insight into the Physics of the Solar Atmosphere

The latest satellite and ground-based observations have provided us a wealth of evidence of waves and oscillations present in the solar atmosphere from the low photosphere to the upper corona. Our understanding of the magnetically dominated solar structures and the dynamics of the solar atmosphere has been considerably improved in light of the high spatial and time resolution observations (e.g. DST/ROSA, IBIS, CoMP, SST/CRISP; SOHO, TRACE, STEREO, Hinode, SDO, etc.) allowing us to perform sub-resolution solar magneto-seismology (SMS) by means of wave and oscillatory data interpreted in the framework of MHD. First I will review the current status of the observed solar MHD waves discovered by these fantastic ground- and space-based facilities.  
Next, I will concentrate on the role of MHD waves, and will discuss the latest status of the sometimes controversial observations of these particular, and fundamentally important magnetic waves. I'll cover the issues related to Alfven waves that has triggered dispute and lively discussions in the community.  
We conclude on how solar magneto-seismology evolved with MHD waves and how the new observational data on waves may be used for more accurate solar and stellar atmospheric diagnostics, including such important aspects as e.g. determining (i) the extent of the force-free (or not!) nature of the magnetised atmosphere, (ii) the geometry, (iii) fine structure, and (iv) even the heating mechanism(s) of solar and stellar coronal plasmas.