File Name : transfer of radiation in spectral lines.pdf Languange Used : English File Size : 44,8 Mb Total Download : 829 **Please Disable Adblock to Show Download Link**
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Author by : C. J. Cannon Languange Used : en Release Date : 2012-01-26 Publisher by : Cambridge University Press ISBN : 9780521106023 File Size : 43,7 Mb Total Download : 702
Originally published in 1985, this monograph describes the interaction of radiation with plasma. Using an approach that is particularly relevant to the interpretation of data from laboratory plasmas or stellar atmospheres, the author sets out the physics and mathematics of the interaction of photons with atoms, molecules, ions and electrons. The emphasis throughout is on relating the formal mathematics to the real world of observable properties and interpretation. The equation of radiative transfer for a two-level atom is solved exactly by two distinct methods. Techniques for solving more real
Author by : R.G. Athay Languange Used : en Release Date : 2012-12-06 Publisher by : Springer Science & Business Media ISBN : 9789401028882 File Size : 42,8 Mb Total Download : 516
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
Author by : John T. Jefferies Languange Used : en Release Date : 1968 Publisher by : ISBN : UCAL:B4264183 File Size : 41,7 Mb Total Download : 870
The purpose of this book is to discuss certain aspects of the theory of the formation and analysis of the line spectrum of a hot gas. The underlying motivation for most of the studies discussed here lies in a desire to develop a physically sound procedure for interpreting the line spectrum of a stellar atmosphere ; correspondingly, the major emphasis is given to problems encountered in astrophysics.