This book discusses key theoretical aspects concerning the formation of the solar wind: the most essential building block in the heliosphere, in which planets orbit. To understand the influence of solar activity on planetary magnetospheres and atmospheres, we need to first understand the origin of the solar wind, which is still under debate. This book presents the outcomes of state-of-the-art numerical simulations of solar wind acceleration, including the first three-dimensional simulation of the turbulence-driven solar wind model. One of the book's goals is to include compressional effects in the dynamics of solar wind turbulence; accordingly, it discusses parametric decay instability in detail. Several key aspects that are relevant to the Parker Solar Probe observations are also discussed. Given its scope, the book plays a key role in bridging the gap between the theory of magnetohydrodynamic turbulence and current/future in-situ observations of the solar wind. This book is based on the Ph.D. thesis by the author, which won the 2019 International Astronomical Union Division E Ph.D. prize.
Fast Solar Wind Driven by Parametric Decay Instability and Alfvén Wave Turbulence
RRP:
$184.00
Description
This book discusses key theoretical aspects concerning the formation of the solar wind: the most essential building block in the heliosphere, in which planets orbit. To understand the influence of solar activity on planetary magnetospheres and atmospheres, we need to first understand the origin of the solar wind, which is still under debate. This book presents the outcomes of state-of-the-art numerical simulations of solar wind acceleration, including the first three-dimensional simulation of the turbulence-driven solar wind model. One of the book's goals is to include compressional effects in the dynamics of solar wind turbulence; accordingly, it discusses parametric decay instability in detail. Several key aspects that are relevant to the Parker Solar Probe observations are also discussed. Given its scope, the book plays a key role in bridging the gap between the theory of magnetohydrodynamic turbulence and current/future in-situ observations of the solar wind. This book is based on the Ph.D. thesis by the author, which won the 2019 International Astronomical Union Division E Ph.D. prize.
Significant advances have been made recently in both the theoretical understanding and observation of small-scale turbulence in different layers of the Sun, and in the instabilities that give rise to...
This is the first book to give a comprehensive overview of recent observational and theoretical results on solar wind structures and fluctuations and magnetohydrodynamic waves and turbulence, ...
WAVE TURBULENCE is a state of a system of many simultaneously excited and interacting waves characterized by an energy distribution which is not in any sense close to thermodynamic equilibrium. Such...
This book provides a systematic introduction to the observation and application of kinetic Alfven waves (KAWs) in various plasma environments, with a special focus on the solar-terrestrial coupling...
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