The book provides a comprehensive overview of the eruptive and wave phenomena in the solar atmosphere. One of the ongoing problems in solar physics is the heating of the solar corona. Currently there is a competition between two mechanisms in explaining the heating, i.e., dissipation of energy by waves and small scale frequent coronal magnetic reconnection. However, some studies indicate this may be a joint effect of these two possible mechanisms. Kelvin–Helmholtz Instability (KHI) of propagating magnetohydrodynamic modes in solar flowing structures plays an important role in the solar atmosphere. It can trigger the onset of wave turbulence leading to effective plasma heating and particle acceleration. KHI is a multifaceted phenomenon and the purpose of this book is to illuminate its (instability) manifestation in various solar jets like spicules, dark mottles, surges, macrospicules, Extreme Ultraviolet (EUV) and X-ray jets, as well as rotating, tornado-like, jets, solar wind, and coronal mass ejections.The modeling of KHI is performed in the framework of ideal magnetohydrodynamics. The book consists of 12 chapters and is intended primarily for advanced undergraduate and postgraduate students, as well as early career researchers.Contents: PrefaceThe Sun: General IntroductionSolar Jets: Origin, Classification and Basic Physical ParametersMagnetohydrodynamic Waves and InstabilitiesNormal Magnetohydrodynamic Modes in Solar JetsKelvin–Helmholtz Instability in Solar SpiculesKelvin–Helmholtz Instability in Solar Photospheric Twisted Flux TubesKelvin–Helmholtz Instability in Solar Surges and Dark MottlesKelvin–Helmholtz Instability in EUV Solar JetsKelvin–Helmholtz Instability in X-ray Solar JetsKelvin–Helmholtz Instability in Rotating Solar JetsKelvin–Helmholtz Instability in Coronal Mass EjectionsSummary and OutlookBibliographyIndex
Readership: Academia, researchers in astrophysics, magnetohydrodynamics.Eruptive and Wave Phenomena in the Solar Atmosphere;MHD Wave and Instabilities;Ideal Magnetohydrodynamics: Basic Equations;Magnetohydrodynamic Waves and Instabilities;Magnetic Reconnection;Solar Flares and Associated Phenomena;Coronal Mass Ejections0Key Features:Clear treatment of major topics, well-illustrated material, and the good agreement between theory and observations
