This book is dedicated to the theory of supernovae, focusing on new computational methods and simulations. It contains three parts: basic principles, numerical methods, and applications. The first part contains a non-formal introduction into the basics of supernovae, Boltzmann kinetic equations — with details of two particles reaction rate calculations — and the transformation of Boltzmann kinetic equations into hydrodynamic elements of statistical physics. It also contains the equation of state for matter of high energy density, with details of calculations for thermodynamic parameters, weak interactions, reaction rate details, and thermonuclear burning. The second part introduces elements of computational physics.The book closes with a presentation of original thought regarding the regime of burning in degenerate carbon-oxygen cores, a neutrino transport in Type II supernovae, a simulation of general relativity (GR) coalescence of neutron stars, aspherical nucleosynthesis in a core-collapse supernova, and thermalization in a pair of plasma winds from a compact strange star.This book brings together generally accepted simulations methods as well as original material written by two respected members of Russian research groups: the Keldysh Institute of Applied Mathematics and Institute of Theoretical and Experimental Physics. It contains the necessary information for a person to start independent research in this fast-developing field, and is therefore an important read for new researchers in this subject.
Relativistic kinetic theory has widespread application in astrophysics and cosmology. The interest has grown in recent years as experimentalists are now able to make reliable measurements on physical systems where relativistic effects are no longer negligible. This ambitious monograph is divided into three parts. It presents the basic ideas and concepts of this theory, equations and methods, including derivation of kinetic equations from the relativistic BBGKY hierarchy and discussion of the relation between kinetic and hydrodynamic levels of description. The second part introduces elements of computational physics with special emphasis on numerical integration of Boltzmann equations and related approaches, as well as multi-component hydrodynamics. The third part presents an overview of applications ranging from covariant theory of plasma response, thermalization of relativistic plasma, comptonization in static and moving media to kinetics of self-gravitating systems, cosmological structure formation and neutrino emission during the gravitational collapse.
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