Turbulence and magnetic fields are ubiquitous in the Universe.
Their importance to astronomy cannot be overestimated. The
theoretical advancements in magnetohydrodynamic (MHD) turbulence
achieved during the past two decades have significantly influenced
many fields of astronomy. This book provides predictive theories of
the magnetic field generation by turbulence and the dissipation of
MHD turbulence. These fundamental non-linear problems were believed
to be tractable only numerically. This book provides complete
analytical descriptions in quantitative agreement with existing
numerics, as well as theoretical predictions in physical regimes
still unreachable by simulations, and explanations of various
related observations. It also discusses and promotes the
astrophysical applications of MHD turbulence theories, including
(i) the particle acceleration and radiation in high-energy
phenomena, e.g., Gamma-Ray Bursts, supernova remnants, cosmic rays;
(ii) interstellar density fluctuations and the effect on
observations, e.g., Faraday rotation, scattering measurements of
Galactic and extragalactic radio sources; (iii) density and
magnetic field structure in molecular clouds toward star formation.
In closing, this book demonstrates the key role of MHD turbulence
in connecting diverse astrophysical processes and unraveling
long-standing astrophysical problems, as foreseen by Chandrasekhar,
a founder of modern astrophysics.
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