Alfvén Waves in the Solar Atmosphere: From Theory to Observations

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Alfvén waves are considered to be viable transporters of the non-thermal energy required to heat the Sun's quiescent atmosphere. An abundance of recent observations, from state-of-the-art facilities, have reported the existence of Alfvén waves in a range of chromospheric and coronal structures. Here, we review the progress made in disentangling the characteristics of transverse kink and torsional linear magnetohydrodynamic (MHD) waves. We outline the simple, yet powerful theory describing their basic properties in (non-)uniform magnetic structures, which closely resemble the building blocks of the real solar atmosphere.
Original languageEnglish
Pages (from-to)1-27
Number of pages27
JournalSpace Science Reviews
Publication statusPublished - Jun 2013


  • Sun: Alfvén waves
  • Sun: chromosphere
  • Sun: corona
  • Sun: spicules
  • Plasma wave heating


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