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By R. M. Goody, Y. L. Yung

A whole revision of Goody's vintage 1964 paintings, this quantity bargains a scientific dialogue of atmospheric radiation strategies that this day are on the heart of globally research and hindrance. It offers with the ways that incident sun radiation is reworked into scattered and thermal radiation, and the thermodynamic results for the Earth's gaseous envelope, settling on facets of the interplay among radiation and atmospheric motions because the vital topic for atmospheric radiation experiences. As an entire therapy of actual and mathematical foundations, the textual content assumes no past wisdom of atmospheric physics. The theoretical dialogue is systematic, and will for this reason be utilized with minor extension to any planetary surroundings.

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Extra resources for Atmospheric Radiation: Theoretical Basis

Example text

SI nomenclature differs from astrophysical nomenclature and is more suited to situations involving finite sources. Equivalents arc specific intensity (this book) and radiance (SI) and flux (this hook) and exitance (SI). This book does not use an equivalent to radiant intensity (SI) and the SI system does not use an equivalent to irradiance (this book) . THEORY OF RADIATIVE TRANSFER 17 FIG. 1. Specific intensity of radiation. direction, where (d, s) denotes the angle between the two vectors. The energy flux across dnd, integrated over all s directions is, from the definitions of IV(P, s) and FVid(P), or where the integral extends over all solid angles.

The polarization ellipse can be defined in terms of the intensities of two components polarized at right angles to each other, and the direction in space of the major or minor axis of the ellipse. Let I and r be two unit vectors forming an orthogonal set with s, the direction of propagation. Let /(v° and /tr) be the intensities of the two polarized components of the beam. The total intensity is and both component intensities are determined if we also know Let tan /3 equal the ratio of the axes of the polarization ellipse, and let x be the angle between 1 and the major axis.

The two processes are distinguished by the sign of the change of radiant intensity as a result of the interaction. If the intensity decreases then we have extinction', if the intensity increases we have emission. No interaction at all can be pictured as the simultaneous extinction and emission of identical quanta, or, alternatively, as a case of vanishingly small interaction coefficients. This prosaic distinction between extinction and emission is the only one that applies to all phenomena described by the two terms.

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