Oxford University Press Inc. , 1984, -718pp. (анг. яз. )
The book divides naturally into three parts; throughout we have attempted to keep the discussion self-contained. In the first part, comprising Chapters 1 to 5, we focus on the dynamics of nonradiating fluids, both ideal and real, classical and relativistic, and then consider applications to a few astrophysically interesting problems: waves, shocks, and stellar winds. As an illustration of numerical methods we outline the basic von Neumann-Richtmyer technique for one-dimensional Lagrangean hydrodynamics. While many of these topics are covered in other books, it is nevertheless necessary to develop them here to the level of completeness, and with the particular emphasis, required to make a meaningful connection to the theory of radiating fluids.
The second part of the book, Chapters 6 to 8, deals with the physics of radiation, radiation transport, and the dynamics of radiating fluids. Here we have attempted to emphasize the very close relationship of radiation hydrodynamics to ordinary fluid dynamics, and to display the underlying unity and strong parallelism of the two formalisms. We therefore approach radiation hydrodynamics as the study of a composite fluid, consisting ofmaterial particles and photons. We develop both the continuum and kinetic-theory views for both matter and radiation, exploiting the conceptual advantages of each in order to paint a complete picture of the physics of the composite radiating fluid. An essential difference between the dynamics of radiating and nonradiating fluids is that because photons typically have much longer mean free paths than their material counter- parts (perhaps approaching or exceeding the physical size of the entire flow), they can introduce a fundamental global coupling between widely separated parts of the flow, which must be treated by a full transport theory. We have attempted to counter what seems to be a commonly held opinion that radiation transport theory is an arcane art, accessible only to specialists, by arguing that conceptually it is simply a nonlocal kinetic theory for a special class of particles (photons) that do not experience body forces but interact strongly with the material component of the fluid locally, while being responsive to the global properties of the flow. We have found this paradigm to be extremely fruitful for our own thinking. Furthermore, we have attempted to show how radiation transport fits naturally into fluid-dynamical computations, in particular how a fully Lagrangean treatment of radiation transport can be incorporated into numerical calculations of one-dimensional flows in both the diffusion and transport regimes. Finally, we discuss a few illustrative examples of astrophysical flows in which radiation plays an important role.
The third part of the book is a short appendix on tensor calculus. We have found that many astronomers and physicists working on radiation hydrodynamics problems are unfamiliar with tensor techniques, and therefore cannot appreciate the power, beauty, and deep physical insight they afford. In the text we exploit tensor concepts to write equations that are covariant by inspection, an approach that allows one to make the transition from ordinary fluids, to relativistic fluids, to radiation almost automatically. The appendix summarizes only the basic material used in the text, and we assume that our readers have this minimum background. Those who do not should read the appendix first; the effort will be amply repaid.
The book divides naturally into three parts; throughout we have attempted to keep the discussion self-contained. In the first part, comprising Chapters 1 to 5, we focus on the dynamics of nonradiating fluids, both ideal and real, classical and relativistic, and then consider applications to a few astrophysically interesting problems: waves, shocks, and stellar winds. As an illustration of numerical methods we outline the basic von Neumann-Richtmyer technique for one-dimensional Lagrangean hydrodynamics. While many of these topics are covered in other books, it is nevertheless necessary to develop them here to the level of completeness, and with the particular emphasis, required to make a meaningful connection to the theory of radiating fluids.
The second part of the book, Chapters 6 to 8, deals with the physics of radiation, radiation transport, and the dynamics of radiating fluids. Here we have attempted to emphasize the very close relationship of radiation hydrodynamics to ordinary fluid dynamics, and to display the underlying unity and strong parallelism of the two formalisms. We therefore approach radiation hydrodynamics as the study of a composite fluid, consisting ofmaterial particles and photons. We develop both the continuum and kinetic-theory views for both matter and radiation, exploiting the conceptual advantages of each in order to paint a complete picture of the physics of the composite radiating fluid. An essential difference between the dynamics of radiating and nonradiating fluids is that because photons typically have much longer mean free paths than their material counter- parts (perhaps approaching or exceeding the physical size of the entire flow), they can introduce a fundamental global coupling between widely separated parts of the flow, which must be treated by a full transport theory. We have attempted to counter what seems to be a commonly held opinion that radiation transport theory is an arcane art, accessible only to specialists, by arguing that conceptually it is simply a nonlocal kinetic theory for a special class of particles (photons) that do not experience body forces but interact strongly with the material component of the fluid locally, while being responsive to the global properties of the flow. We have found this paradigm to be extremely fruitful for our own thinking. Furthermore, we have attempted to show how radiation transport fits naturally into fluid-dynamical computations, in particular how a fully Lagrangean treatment of radiation transport can be incorporated into numerical calculations of one-dimensional flows in both the diffusion and transport regimes. Finally, we discuss a few illustrative examples of astrophysical flows in which radiation plays an important role.
The third part of the book is a short appendix on tensor calculus. We have found that many astronomers and physicists working on radiation hydrodynamics problems are unfamiliar with tensor techniques, and therefore cannot appreciate the power, beauty, and deep physical insight they afford. In the text we exploit tensor concepts to write equations that are covariant by inspection, an approach that allows one to make the transition from ordinary fluids, to relativistic fluids, to radiation almost automatically. The appendix summarizes only the basic material used in the text, and we assume that our readers have this minimum background. Those who do not should read the appendix first; the effort will be amply repaid.