Titlebook: Radiative Transfer; An Introduction to E Hélène Frisch Book 2022 The Editor(s) (if applicable) and The Author(s), under exclusive license t

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書目名稱Radiative Transfer影響因子(影響力)




書目名稱Radiative Transfer影響因子(影響力)學(xué)科排名




書目名稱Radiative Transfer網(wǎng)絡(luò)公開度




書目名稱Radiative Transfer網(wǎng)絡(luò)公開度學(xué)科排名




書目名稱Radiative Transfer被引頻次




書目名稱Radiative Transfer被引頻次學(xué)科排名




書目名稱Radiative Transfer年度引用




書目名稱Radiative Transfer年度引用學(xué)科排名




書目名稱Radiative Transfer讀者反饋




書目名稱Radiative Transfer讀者反饋學(xué)科排名

Dissonance

Conservative Scattering: The Milne Problemion obtained in Chap. . to derive an exact expression of the source function. For monochromatic scattering, we show how to express it in terms of the Hopf function and describe the properties of the latter.

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The Case Eigenfunction Expansion Method The eigenfunctions are used to expand arbitrary solutions, and the main task consists of the determination of the expansion coefficients. In this Chapter, this method referred as the Case expansion method, is applied to radiative transfer equations for monochromatic scattering and complete frequency redistribution.

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The ,-law and the Nonlinear ,-Equationey do not make use of complex plane analysis, whether they are really elementary, is a matter of appreciation. A certain advantage of these methods is that there is in general no need to distinguish between monochromatic scattering and complete frequency redistribution.

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Coordinate

Conservative Rayleigh Scattering: Exact Solutionsne (a matrix Riemann–Hilbert problem), which is then decomposed into two scalar Riemann–Hilbert problems. The decomposition method closely follows the 1967 approach of C. Siewert and S. Fraley. The two scalar problems, solved with the method described in Chapter 5, provide the functions ..(.) and ..(.).

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Book 2022al methods, providing exact expressions for the radiation field in a semi-infinite atmosphere, are described in detail and applied to unpolarized and polarized continuous spectra and spectral lines. Among these methods, the Wiener–Hopf method, introduced in 1931 for a stellar atmospheric problem, is

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