2015/03/04 by D. B. Jess, R. J. Morton, G. Verth +5 · 2 citations
Physics and Astronomy · #Astro and Planetary Science #Astrobiology #Astronomy #Astrophysics #Chromosphere #Corona (planetary geology) #Coronal hole #Coronal mass ejection #Coronal radiative losses #Magnetic field #Magnetohydrodynamic drive #Magnetohydrodynamics #Nanoflares #Photosphere #Physics #Plasma #Solar and Space Plasma Dynamics #Solar atmosphere #Solar wind #Spectral line #Stellar, planetary, and galactic studies #astro-ph.SR
paper · pdf · doi:10.1007/s11214-015-0141-3
48 pages, 25 figures, accepted into Space Science Reviews
openalex publication_date 2015/03/04 · arxiv created 2015/03/11 · arxiv updated 2015/03/12 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
The chromosphere is a thin layer of the solar atmosphere that bridges the relatively cool photosphere and the intensely heated transition region and corona. Compressible and incompressible waves propagating through the chromosphere can supply significant amounts of energy to the interface region and corona. In recent years an abundance of high-resolution observations from state-of-the-art facilities have provided new and exciting ways of disentangling the characteristics of oscillatory phenomena propagating through the dynamic chromosphere. Coupled with rapid advancements in magnetohydrodynamic wave theory, we are now in an ideal position to thoroughly investigate the role waves play in supplying energy to sustain chromospheric and coronal heating. Here, we review the recent progress made in characterising, categorising and interpreting oscillations manifesting in the solar chromosphere, with an impetus placed on their intrinsic energetics.