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Fast solar wind driven by parametric decay instability and Alfvén wave turbulence / Munehito Shoda.

9789811610301 (electronic bk.)
9811610304 (electronic bk.)
9789811610295

Singapore : Springer, [2021]

English

1 online resource (xv, 94 pages) : illustrations (chiefly color)

10.1007/978-981-16-1030-1 doi

QB529

523.5/8

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.

"Doctoral thesis accepted by The University of Tokyo, Tokyo, Japan."

Includes bibliographical references.

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Online resource; title from PDF title page (SpringerLink, viewed April 22, 2021).

Springer theses. 2190-5053

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