2012/10/12 by Mihalis Mathioudakis, M. Mathioudakis, D. B. Jess +3 · 6 citations
Biochemistry, Genetics and Molecular Biology · Physics and Astronomy · #Astro and Planetary Science #Astrobiology #Astronomy #Astrophysics #Atmosphere (unit) #Computational physics #Corona (planetary geology) #Coronal hole #Coronal loop #Coronal mass ejection #Geomagnetism and Paleomagnetism Studies #Magnetic field #Magnetohydrodynamic drive #Magnetohydrodynamics #Meteorology #Physics #Planetary science #Solar and Space Plasma Dynamics #Solar atmosphere #Solar wind #Thermal #astro-ph.SR
paper · pdf · doi:10.1007/s11214-012-9944-7
Space Science Reviews, accepted
arxiv created 2012/10/12 · openalex publication_date 2012/11/09 · arxiv updated 2015/06/11 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Alfven 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 Alfven 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.