Magnetohydrodynamic waves in open coronal structures
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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 (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.
Banerjee , D , Krishna Prasad , S , Pant , V , McLaughlin , J A , Antolin , P , Magyar , N , Ofman , L , Tian , H , Van Doorsselaere , T , De Moortel , I & Wang , T J 2021 , ' Magnetohydrodynamic waves in open coronal structures ' , Space Science Reviews , vol. 217 , no. 7 , 76 . https://doi.org/10.1007/s11214-021-00849-0
Space Science Reviews
Copyright © 2021 the Author(s), under exclusive licence to Springer Nature B.V. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the author created accepted manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1007/s11214-021-00849-0.
DescriptionFunding: 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.
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