Chromospheric and Coronal Wave Generation in a Magnetic Flux Sheath
Informazioni aggiuntive
Autori
Kato Y.,
Steiner O.,
Hansteen V.,
Gudiksen B. a.
Tipo
Articolo pubblicato in rivista scientifica
Anno
2016
Lingua
Inglese
Abstract
Using radiation magnetohydrodynamic simulations of the solar atmosphericlayers from the upper convection zone to the lower corona, we investigate the self-consistent excitation of slow magneto-acoustic body waves (slow modes) in a magnetic flux concentration. We find that the convective downdrafts in the close surroundings of a two-dimensional flux slab łdquopumprdquo the plasma inside it in the downward direction. This action produces a downflow inside the flux slab, which encompasses ever higher layers, causing an upwardly propagating rarefaction wave. The slow mode, excited by the adiabatic compression of the downflow near the optical surface, travels along the magnetic field in the upward direction at the tube speed. It develops into a shock wave at chromospheric heights, where it dissipates, lifts the transition region, and produces an offspring in the form of a compressive wave that propagates further into the corona. In the wake of downflows and propagating shock waves, the atmosphere inside the flux slab in the chromosphere and higher tends to oscillate with a period of $nu$ ap 4 mHz. We conclude that this process of łdquomagnetic pumpingrdquo is a most plausible mechanism for the direct generation of longitudinal chromospheric and coronal compressive waves within magnetic flux concentrations, and it may provide an important heat source in the chromosphere. It may also be responsible for certain types of dynamic fibrils.
Rivista
Astrophysical Journal
Volume
827
Pagina inizio
7
Parole chiave
irsol-refereed-scientific-papers
