Kelvin-Helmholtz Instability Solar Atmhb: Kelvin-Helmholtz Instability in Solar Atmospheric Jets

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 Preface 1. The Sun: General Introduction 1.1 Internal structure 1.1.1 Core 1.1.2 Radiative zone 1.1.3 Convective zone 1.2 External structure 1.2.1 Photosphere 1.2.2 Chromosphere 1.2.3 Corona 1.3 Quiet and active Sun 1.3.1 Prominences/Filaments 1.3.2 Solar flares 1.3.3 Solar jets 1.3.4 Coronal mass ejections 1.4 Solar cycle 1.5 Solar eruption mechanisms 2. Solar Jets: Origin, Classification and Basic Physical Parameters 2.1 Classification 2.2 Basic physical parameters 3. MagnetohydrodynamicWaves and Instabilities 3.1 Magnetohydrodynamics basic equations 3.2 Magnetohydrodynamic equilibrium 3.3 Magnetic reconnection 3.4 Magnetohydrodynamic waves 3.4.1 MHD modes in magnetic flux tubes 3.5 Magnetohydrodynamic instabilities 3.5.1 Rayleigh–Taylor instability 3.5.2 Kelvin–Helmholtz instability 3.5.3 Sausage and kink instabilities 4. Normal Magnetohydrodynamic Modes in Solar Jets 4.1 Jet geometry, basic MHD equations, and wave dispersion relation 4.1.1 Derivation of wave dispersion relation on using the operator coefficient techniques 4.2 An example for finding unstable solutions to the wave dispersion relation 5. Kelvin–Helmholtz Instability in Solar Spicules 5.1 Geometry and the wave dispersion relations 5.1.1 Dispersion diagrams of kink waves 5.1.2 Dispersion diagrams of sausage waves 6. Kelvin–Helmholtz Instability in Solar Photospheric Twisted Flux Tubes 6.1 Introduction 6.2 Geometry, the basic MHD equations, and the wave dispersion relation 6.3 Numerical solutions and wave dispersion diagrams 7. Kelvin–Helmholtz Instability in Solar Surges and Dark Mottles 7.1 Kelvin–Helmholtz instability in solar surges 7.1.1 Surge models, basic parameters, and governing equations 7.1.2 Wave dispersion relations 7.1.3 Numerical calculations and results 7.2 Kelvin–Helmholtz instability in dark mottles 7.2.1 Mottles models, basic parameters, and governing equations 7.2.2 Numerical calculations and results 7.2.3 Discussion and conclusion 8. Kelvin–Helmholtz Instability in EUV Solar Jets 8.1 Observations, nature, and physical parameters of EUV jets 8.2 Jets geometry and the governing magnetohydrodynamic equations 8.3 Kelvin–Helmholtz instability in an EUV jet observed by Hinode 8.3.1 Kelvin–Helmholtz instability of the kink (m = 1) mode 8.3.2 Kelvin–Helmholtz instability of the m = 2, 3, and 4 modes 8.4 Kelvin–Helmholtz instability in an EUV jet observed by SDO/AIA 9. Kelvin–Helmholtz Instability in X-ray Solar Jets 9.1 Observations and nature of the X-ray jets 9.2 Magnetic field topology, physical parameters, and MHD wave dispersion relations 9.2.1 Kelvin–Helmholtz instability of MHD modes in untwisted flux tubes 9.2.2 Kelvin–Helmholtz instability of MHD modes in twisted flux tubes 10. Kelvin–Helmholtz Instability in Rotating Solar Jets 10.1 Observations and nature of the rotating solar jets 10.2 The geometry, magnetic field, and physical parameters in a jet model 10.3 Wave dispersion relation 10.4 Numerical solutions, wave dispersion, and growth rate diagrams 10.4.1 Kelvin–Helmholtz instability in a standard polar coronal hole jet 10.4.2 Kelvin–Helmholtz instability in a blowout polar coronal hole jet 10.4.3 Kelvin–Helmholtz instability in a jet emerging from a filament eruption 10.4.4 Kelvin–Helmholtz instability in a spinning macrospicule 10.5 Summary 11. Kelvin–Helmholtz Instability in Coronal Mass Ejections 11.1 Coronal mass ejections and magnetic flux ropes 11.2 Kelvin–Helmholtz instability in coronal mass ejections 11.3 Numerical solutions and wave dispersion diagrams 12. Summary and Outlook Bibliography Index "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"--Publisher's website