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Get Atmosphere, Ocean and Climate Dynamics: An Introductory Text PDF

By John Marshall

ISBN-10: 0080556701

ISBN-13: 9780080556703

ISBN-10: 0125586914

ISBN-13: 9780125586917

For complex undergraduate and starting graduate scholars in atmospheric, oceanic, and weather technological know-how, surroundings, Ocean and weather Dynamics is an introductory textbook at the circulations of the ambience and ocean and their interplay, with an emphasis on international scales. it's going to supply scholars a great grab of what the ambience and oceans seem like at the large-scale and why they appear that manner. The function of the oceans in weather and paleoclimate is additionally mentioned. the mix of observations, conception and accompanying illustrative laboratory experiments units this article aside by way of making it obtainable to scholars without previous education in meteorology or oceanography. * Written at a mathematical point that's beautiful for undergraduates andbeginning graduate scholars* presents an invaluable academic device via a mix of observations andlaboratory demonstrations which might be considered over the internet* includes directions on the way to reproduce the straightforward yet informativelaboratory experiments* contains copious difficulties (with pattern solutions) to assist scholars research thematerial.

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Additional info for Atmosphere, Ocean and Climate Dynamics: An Introductory Text

Example text

An ‘‘opaque’’ greenhouse made up of two layers of atmosphere. Each layer completely absorbs the IR radiation impinging on it. 2)—and do the required budgets for each layer and at the surface (we are not going to do this). An incomplete schematic of how this might look for a rather opaque atmosphere is shown in Fig. 10. The resulting profile, which would be the actual mean atmospheric temperature profile if heat transport in the atmosphere occurred only through radiative transfer, is known as the radiative equilibrium temperature profile.

2. Atmospheric layers Coming down from the top of the atmosphere, the first hot spot evident in Fig. 1 is the thermosphere, where the temperature is very high and variable. It is here that very short wavelength UV is absorbed by oxygen (cf. 2), thus heating the region. 1 μm). Therefore, because of the scarcity of polyatomic molecules, IR loss of energy is weak, so the temperature of the region gets very high (as high as 1000 K). The air is so tenuous that assumptions of local thermodynamic equilibrium, as in blackbody radiation, are not applicable.

8) was doubled, but albedo remained fixed at 30%? 2. Suppose that the Earth is, after all, flat. Specifically, consider it to be a thin circular disk (of radius 6370 km), orbiting the Sun at the same distance as the Earth; the planetary albedo is 30%. The vector normal to one face of this disk always points directly towards the Sun, and the disk is made of perfectly conducting material, so both faces of the disk are at the same temperature. Calculate the emission temperature of this disk, and compare with Eq.

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Atmosphere, Ocean and Climate Dynamics: An Introductory Text by John Marshall


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