Fast Solar Wind Driven by Parametric Decay Instability and Alfvén Wave Turbulence

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.

Nominated as an outstanding PhD thesis by the University of Tokyo, Tokyo, Japan Is a winner of the 2019 International Astronomical Union Division E Ph.D. prize Includes the first-ever 3D simulation of the turbulence-driven solar wind model Shares new insights into the nature of compressible MHD turbulence in the solar wind Bridges the gap between current and future observations of the solar wind on the one hand, and corresponding theory on the other

Inhalt
General Introduction.- 1D model with Compressional and Non-compressional Nonlinear Effects.- Onset and Suppression of Parametric Decay Instability.- 3D Simulations of the Fast Solar Wind.- Summary and Discussion.