Skip to main content

Magnetohydrodynamic Waves in Open Coronal Structures


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.

This is a preview of subscription content, access via your institution.

Fig. 1
Fig. 2
Fig. 3
Fig. 4
Fig. 5
Fig. 6
Fig. 7
Fig. 8
Fig. 9
Fig. 10
Fig. 11


Download references


The authors thank the anonymous referees for their helpful suggestions. We wish to acknowledge ISSI-BJ for hosting the workshop at Beijing and for their generous Support for all the participants. SKP is grateful to FWO Vlaanderen for a senior postdoctoral fellowship (No. 12ZF420N). VP was supported by the Spanish Ministerio de Ciencia, Innovación y Universidades through project PGC2018-102108-B-I00 and FEDER funds. VP and TVD are supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 724326). J.A.M. acknowledges UK Science and Technology Facilities Council (STFC) support from grant ST/T000384/1. L.O. acknowledges support by NASA grants NNX16AF78G, 80NSSC18K1131 and NASA Cooperative Agreement NNG11PL10A to CUA. P.A. acknowledges funding from his STFC Ernest Rutherford Fellowship (No. ST/R004285/2). IDM acknowledges support from the UK Science and Technology Facilities Council (consolidated grants ST/N000609/1 and ST/S000402/1), the European Union Horizon 2020 research and innovation programme (grant agreement No. 647214) and the Research Council of Norway through its Centres of Excellence scheme, project number 262622. H.T. is supported by NSFC grants 11825301 and 11790304(11790300). T.J.W. acknowledges support by NASA grants 80NSSC18K1131, 80NSSC18K0668, and NASA Cooperative Agreement NNG11PL10A to CUA.

Author information

Authors and Affiliations


Corresponding author

Correspondence to D. Banerjee.

Additional information

Publisher’s Note

Springer Nature remains neutral with regard to jurisdictional claims in published maps and institutional affiliations.

Oscillatory Processes in Solar and Stellar Coronae

Edited by Valery M. Nakariakov, Dipankar Banerjee, Bo Li, Tongjiang Wang, Ivan Zimovets and Maurizio Falanga

Rights and permissions

Reprints and Permissions

About this article

Verify currency and authenticity via CrossMark

Cite this article

Banerjee, D., Krishna Prasad, S., Pant, V. et al. Magnetohydrodynamic Waves in Open Coronal Structures. Space Sci Rev 217, 76 (2021).

Download citation

  • Received:

  • Accepted:

  • Published:

  • DOI:


  • Solar corona
  • Magnetohydrodynamics
  • Waves and oscillations