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ISSN Online: 2377-424X

International Heat Transfer Conference 5
September, 3-7, 1974, Tokyo, Japan

ENERGY TRANSFER IN PLANETARY ATMOSPHERES

Get access (open in a dialog) DOI: 10.1615/IHTC5.2620
pages 61-71

Resumo

The purpose of this paper is to present analytical models for describing infrared gaseous radiation which are based upon methods employed in both engineering and atmospheric physics, to illustrate their application to specific planetary atmospheres, and to compare the resulting thermal structure or energy balance results with observational data.
Consideration is first given to the atmospheres of Mars and Venus, which are composed primarily of carbon dioxide. Radiative transfer within the stratospheres and mesospheres of these planets results from infrared-active bands, and these atmospheres serve as a convenient vehicle for illustrating effects such as Doppler broadening and vibrational nonequilibrium, as well as the influence of hot bands and minor isotope bands.
The primary infrared opacity of the atmospheres of the major planets, on the other hand, is due to pressure-induced absorption by hydrogen, with infrared-active bands of hydrocarbon gases constituting a secondary source of opacity. Employing simple analytical models for these opacity sources, possible model atmospheres are discussed in light of ground-based data for Jupiter and Saturn.
The final atmosphere to be considered is that of Earth, for which the primary infrared opacity is due to water vapor. Particular attention here is directed towards the sensitivity of the Earth's surface temperature to factors such as planetary albedo and cloudiness.