  Macroscopic wave and oscillatory phenomena ubiquitously detected in the
plasma of the corona of the Sun are interpreted in terms of magnetohydrodynamic
theory. Fast and slow magnetoacoustic waves are clearly distinguished in
observations. Properties of coronal magnetohydrodynamic waves are determined by
local parameters of the plasma, including the field-aligned filamentation
typical for the corona. It makes coronal magnetohydrodynamic waves reliable
probes of the coronal plasma structures by the method of magnetohydrodynamic
seismology. For example, propagating slow waves indicate the local direction of
the guiding magnetic field. Standing, sloshing and propagating slow waves can
be used for probing the coronal heating function and the polytropic index. Kink
oscillations of coronal plasma loops provide us with the estimations of the
absolute value of the magnetic field in oscillating plasma loops. This tutorial
introduces several techniques of magnetohydrodynamic seismology of solar
coronal plasmas. It includes the description of practical steps in the data
acquisition, pre-processing, and processing using the open-access data of the
Atmospheric Imaging Assembly on the Solar Dynamics Observatory spacecraft, and
elaborated data analysis techniques of motion magnification and Bayesian
statistics.
