Space Science Reviews

, Volume 175, Issue 1–4, pp 1–27 | Cite as

Alfvén Waves in the Solar Atmosphere

From Theory to Observations
Article

Abstract

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.

Keywords

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

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© Springer Science+Business Media Dordrecht 2012

Authors and Affiliations

  1. 1.Astrophysics Research Centre, School of Mathematics and PhysicsQueen’s University BelfastBelfastUK
  2. 2.Solar Physics & Space Plasma Research Centre (SP²RC), School of Mathematics and StatisticsUniversity of SheffieldSheffieldUK

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