Magnetohydrodynamic Waves in Open Coronal Structures

doi:10.1007/s11214-021-00849-0

Magnetohydrodynamic Waves in Open Coronal Structures

2021-09-21

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DOI：10.1007/s11214-021-00849-0

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Modern observatories have revealed the ubiquitous presence of magnetohydrodynamic waves in the solar corona. The propagating waves (in contrast to the standing waves) are usually originated in the lower solar atmosphere which makes them particularly relevant to coronal heating. Furthermore, open coronal structures are believed to be the source regions of solar wind, therefore, the detection of MHD waves in these structures is also pertinent to the acceleration of solar wind. Besides, the advanced capabilities of the current generation telescopes have allowed us to extract important coronal properties through MHD seismology. The recent progress made in the detection, origin, and damping of both propagating slow magnetoacoustic waves and kink (Alfvenic) waves is presented in this review article especially in the context of open coronal structures. Where appropriate, we give an overview on associated theoretical modelling studies. A few of the important seismological applications of these waves are discussed. The possible role of Alfvenic waves in the acceleration of solar wind is also touched upon.

Keywords:

Solar corona

Magnetohydrodynamics

Waves and oscillations

Magnetohydrodynamic Waves in Open Coronal Structures

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