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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.
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