Magnetohydrodynamic Waves in Open Coronal Structures

Dipankar Banerjee*, S. Krishna Prasad, Vaibhav Pant, James McLaughlin, Patrick Antolin, N. Magyar, Leon Ofman, H. Tian, Tom Van Doorsselaere, Ineke de Moortel, T. J. Wang

*Corresponding author for this work

Research output: Contribution to journalReview articlepeer-review

44 Citations (Scopus)
23 Downloads (Pure)


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 (Alfvénic) 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 Alfvénic waves in the acceleration of solar wind is also touched upon.

Original languageEnglish
Article number76
Number of pages37
JournalSpace Science Reviews
Issue number7
Early online date21 Sept 2021
Publication statusPublished - 1 Oct 2021


Dive into the research topics of 'Magnetohydrodynamic Waves in Open Coronal Structures'. Together they form a unique fingerprint.

Cite this