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

This book discusses the theoretical aspects of the solar wind, including its formation, acceleration, and turbulence. It presents state-of-the-art numerical simulations and discusses their relevance to Parker Solar Probe observations.

Format: Paperback / softback
Length: 94 pages
Publication date: 15 April 2022
Publisher: Springer Verlag, Singapore

This comprehensive work delves into the intricate theoretical aspects surrounding the formation of the solar wind, a fundamental component of the heliosphere, in which planets orbit. To comprehend the profound impact of solar activity on planetary magnetospheres and atmospheres, it is essential to delve into the origins of the solar wind, a topic that remains subject to ongoing debate. This book presents the results of cutting-edge numerical simulations that explore the mechanisms of solar wind acceleration, encompassing the first-ever three-dimensional simulation of a turbulence-driven solar wind model. One of the primary objectives of this book is to incorporate compressional effects into the dynamics of solar wind turbulence, thereby providing a detailed examination of parametric decay instability. Furthermore, the book addresses several key aspects that are of significant relevance to the observations made by the Parker Solar Probe. Given the broad scope of its content, this book assumes a pivotal role in bridging the gap between the theory of magnetohydrodynamic turbulence and the current and future in-situ observations of the solar wind.

The foundation of this book is rooted in the author's Ph.D. thesis, which secured the prestigious 2019 International Astronomical Union Division E Ph.D. prize. Through meticulous research and analysis, the author has unraveled the complexities of solar wind formation, offering valuable insights into this celestial phenomenon.

Weight: 185g
Dimension: 235 x 155 (mm)
ISBN-13: 9789811610325
Edition number: 1st ed. 2021