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Titlebook: Radiation Transport in Spectral Lines; R. Grant Athay Book 1972 D. Reidel Publishing Company, Dordrecht, Holland 1972 atmosphere.star.turb

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书目名称Radiation Transport in Spectral Lines
编辑R. Grant Athay
视频video
丛书名称Geophysics and Astrophysics Monographs
图书封面Titlebook: Radiation Transport in Spectral Lines;  R. Grant Athay Book 1972 D. Reidel Publishing Company, Dordrecht, Holland 1972 atmosphere.star.turb
描述The usual book on the theory of spectral line formation begins with an in-depth dis­ cussion of radiation transfer, including the elegant methods of obtaining analytical solutions for special cases, and of the physics of line broadening. Neither of those features will be found in this book. It is assumed that the reader is already familiar with the essentials of transport theory and of line broadening and is ready to investi­ gate some of the particular applications of the theory to the flow of line photons through the outer layers of a star, or other tenuous media. The main thrust of this book is toward the compilation and presentation of a vast quantity of computational material available to the author in the form of computer output. The material presented represents a highly filtered sample of the published work in this subject plus an extensive set of previously unpublished results. To present large quantities of computer output in an intelligible and efficient way is a difficult task, for which I have found no really satisfactory solution. Chapters III and IV, in particular, contain almost exclusively this type of presentation. The reader may find these chapters somewhat tedio
出版日期Book 1972
关键词atmosphere; star; turbulence
版次1
doihttps://doi.org/10.1007/978-94-010-2888-2
isbn_softcover978-90-277-0241-8
isbn_ebook978-94-010-2888-2
copyrightD. Reidel Publishing Company, Dordrecht, Holland 1972
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The Line Source Function,In this chapter we shall have need of the following quantities and relationships in addition to those defined in Chapter I:... = profile of .. normalized to unit area.
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Line Profiles,The specific intensity at frequency ν coming from a position . on a stellar disk is given by.For .. of the form.Equation (V-l) gives.so that.Equation (V-4) is the familiar Eddington-Barbier relation widely used in solar applications for inversion of the integral in Equation (V-1).
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