Structuring of the Solar Plasma by the Magnetic Field

Abstract

This paper presents a simplified overview of the role of the magnetic field in the solar atmosphere. The magnetic field emanating from the solar interior governs energy transport and plasma motions in the outer solar atmosphere. Thereby it creates structure, such as coronal holes, loops and prominences, and the dynamical phenomena known as coronal mass ejections and flares. The magnetic field is also thought to be at the origin of the coronal heating, so of the corona itself. An overview of atmospheric structure is presented, followed by illustrations on present ideas on the interaction between plasma and magnetic field. The physical conditions in the corona are briefly compared to those in the magnetosphere. The emphasis is then put on the energetic processes from the largest ones (coronal mass ejections) over flares and X-ray bright points to coronal heating. In all cases magnetic reconnection is likely to play a key role. Solar prominences are then described because their observations provide important information on the surrounding coronal magnetic field. Finally the implications of processes in the convection zone on the physics of the corona and of the interplanetary medium are illustrated for the case of formation, storage and ejection of twisted magnetic flux tubes.KeywordsSolar WindCurrent SheetCoronal Mass EjectionSolar PhysCoronal HoleThese keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.