http://arxiv.org/abs/2204.06010
Solar flares and coronal mass ejections are the largest energy release phenomena in the current solar system. They cause drastic enhancements of electromagnetic waves of various wavelengths and sometimes eject coronal material into the interplanetary space, disturbing the magnetic surroundings of orbiting planets including the Earth. It is generally accepted that solar flares are a phenomenon in which magnetic energy stored in the solar atmosphere above an active region is suddenly released through magnetic reconnection. Therefore, to elucidate the nature of solar flares, it is critical to estimate the complexity of the magnetic field and track its evolution. Magnetic helicity, a measure of the twist of coronal magnetic structures, is thus used to quantify and characterize the complexity of flare-productive active regions. This chapter provides an overview of solar flares and discusses how the different concepts of magnetic helicity are used to understand and predict solar flares.
S. Toriumi and S. Park
Thu, 14 Apr 22
57/62
Comments: 42 pages, 13 figures, to appear as a chapter in the AGU book “Helicities in Geophysics, Astrophysics and Beyond”