MHD seismology of the solar corona

TL;DRAbstract

The Sun’s interior is a region of high β because the gas pressure there is quite high. By contrast, the rapid decrease in gas pressure in the upper layers of the solar atmosphere suggests that β is of the order of unity or smaller there, and so magnetic effects are significant. The idea of remote diagnostics of the Sun with observationally determined properties of waves has been successfully realized in helioseismology. Measurement of parameters of acoustic waves through various layers of the Sun’s interior, makes it possible to reconstruct the physical conditions in these parts of the Sun which is non-observable by usual methods. By contrast, the solar corona is observable in the entire spectrum of electromagnetic radiation and particle emissions. However, the coronal physical conditions, for instance, rarefied, weakly collisional and almost ionized plasma, highly structured by the magnetic field, complicate the observational investigation of the corona. Some of the physical parameter

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