Alfvén Waves in the Solar Atmosphere

By M. Mathioudakis, D. Jess, R. Erdélyi. 2012

166 citations recorded by the source corpus.

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.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/273c13963c3f98fad8cf10b31d90bfd43a05c394

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Citations in the corpus

Magnetohydrodynamic Oscillations in the Solar Corona and Earth’s Magnetosphere: Towards Consolidated Understanding (2016, background): “…(2008), Petrosyan et al. (2010), Banerjee et al. (2011), Patsourakos and Vourlidas (2012), De Moortel and Nakariakov (2012), Stepanov et al. (2012), Mathioudakis et al. (2013), Liu and Ofman (2014) for most recent “solar” reviews, and Guglielmi and Pokhotelov (1996), Walker (2005), Alperovich and…”
Multiwavelength Studies of MHD Waves in the Solar Chromosphere (2015, background): “Such detailed overviews include quasi-periodic (Nakariakov et al. 2005), standing (Wang 2011), magnetoacoustic (Van Doorsselaere et al. 2009b; De Moortel 2009) and Alfvén (Mathioudakis et al. 2013) waves.”