Cyril Ponnamperuma's Chemical Evolution of the Giant Planets PDF

By Cyril Ponnamperuma

ISBN-10: 0125613504

ISBN-13: 9780125613507

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There remains some unidentified absorption in the range 10,200 10,700 Â. 65 ym. One may speculate that some of the photolysis products are responsible, but such possibilities are limited because most compounds must condense at the low temperature of Titan's atmosphere. The best candidates are 30 TITAN'S ATMOSPHERE AND SURFACE therefore C2H5, C2H4, and C2H2, and perhaps CH3NH2 if ammonia photolysis occurs. Not enough is known about the spectra of any of these compounds for an identification or rejection.

The coefficient 3 for absorption by N 2 is much smaller than for CH^ (Bosomworth and Gush, 1965). Such absorption would therefore be important only for a large excess of nitrogen. If the surface temperature is 125°K, the temperature profile could lie between the two shown in Fig. M. HUNTEN saturated and dry adiabats. Clouds are shown opposite the upper portion of the saturated adiabat, but could extend lower. The temperature at the tropopause should be somewhere between the observed 82°K brightness temperature at 34 ym (Table I) and the GoId-Humphreys skin temperature, 72°K.

Previously, Axel (1972) had applied similar reasoning to Jupiter. If the dust particles are small, they are poor infrared radiators, and in a vacuum they can become much hotter than the equilibrium temperature for a large body. In an atmosphere, their heat is primarily transferred to the gas, and radiated in the methane and ethane bands that are observed. There is also some optically thin continuous emission by the dust. , 1973; Caldwell, 1974) the brightness temperature of 125°K around 10 urn is attributed to this dust emission, instead of the surface as assumed here.

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Chemical Evolution of the Giant Planets by Cyril Ponnamperuma


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