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MHD Waves in Coronal Holes

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dc.contributor.author Banerjee, D
dc.contributor.author Krishna Prasad, S
dc.date.accessioned 2020-11-20T13:15:23Z
dc.date.available 2020-11-20T13:15:23Z
dc.date.issued 2015-05
dc.identifier.citation Andreas Keiling, Dong-Hun Lee, Valery Nakariakov (Eds). Low-frequency waves in space plasmas, pp. 419-430 en_US
dc.identifier.isbn 978-1-119-05495-5
dc.identifier.uri http://prints.iiap.res.in/handle/2248/7307
dc.description Restricted Access © American Geophysical Union http://dx.doi.org/10.1002/9781119055006.ch24 en_US
dc.description.abstract Coronal holes are the dark patches in the solar corona associated with relatively cool, less dense plasma and unipolar fields. The fast component of the solar wind emanates from these regions. Several observations reveal the presence of magnetohydrodynamic (MHD) waves in coronal holes which are believed to play a key role in the acceleration of fast solar wind. The recent advent of high-resolution instruments had brought us many new insights on the properties of MHD waves in coronal holes which are reviewed in this article. The advances made in the identification of compressive slow MHD waves in both polar and equatorial coronal holes, their possible connection with the recently discovered highspeed quasi-periodic upflows, their dissipation, and the detection of damping in Alfv´en waves from the spectral line width variation are discussed in particular. en_US
dc.language.iso en en_US
dc.publisher John Wiley & Sons, Inc. en_US
dc.subject Compressive waves en_US
dc.subject Coronal holes en_US
dc.subject Imaging techniques en_US
dc.subject Incompressive waves en_US
dc.subject Magnetohydrodynamic waves en_US
dc.subject Spectroscopic techniques en_US
dc.subject Wave damping en_US
dc.title MHD Waves in Coronal Holes en_US
dc.type Book chapter en_US


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