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Additional resources for An Introduction to Atmospheric Radiation
The Lorentz shape of infrared lines is fundamental for the theory of infrared radiative transfer in the atmosphere. Thus it is desirable to give a brief explanation of how the formula denoted in Eq. 34) is derived. 36a) where A is an arbitrary amplitude. During the period - tl2 to t12, the distribution of amplitude g(v) of the wave in the discrete frequency domain may be obtained from the Fourier cosine transform as follows: g(v) = ~ f ~/ 2 (A cos 2nv ot') cos 2nvt' dt' = _A_ [sin n(v o + v)t (2n)3/2 VA +v + sin n(v o - V)tJ.
14 The contrast of the object against its surroundings is defined by where B represents the brightness of the object and B o the brightness of the background sky. By these definitions, B = B o when x ---+ 00, whereas B = 0 when x = 0, where x denotes the distance between the object and the observer. 02. 912//3. 15 In reference to Fig. (SI)? 16 By differentiation with respect to the optical thickness r show that Eqs. 65) reduce to Eq. 63), the equation of transfer for plane parallel atmospheres.
If observations of the monochromatic irradiance are carried out for wavelengths covering the entire solar spectrum, then from Eq. 8) where N is the total number of the monochromatic irradiance measured. 4 43 Determinations of the Solar Constant In F AO <, <, <, t -« u, ~ 2 4 m = sec eo 6 Fig. 8 Hypothetical observed monochromatic solar irradiances FA as a function of the effective path length. 9) The foregoing outlines theoretical procedures of the Smithsonian long method for the determination of the solar constant.