THE EMISSIVITY OF VOLATILE ICES ON TRITON AND PLUTO

The Hapke theory is used to calculate the emissivity of a semi-infinit e layer of granular N-2 ice with CH4 and CO as contaminants. It is ass umed that the layer is composed of grains which can be characterized a s having a single size, and that temperature gradients in the emitting layers of the surface are negligible. The emission spectrum for beta- N-2, stable above 35.6 K, results from a very broad peak in the absorp tion spectrum centered at 154 mu m, while two absorption peaks, at 143 and 204 mu m, produce the emission spectrum of the lower temperature alpha-N-2 phase. For a grain size of 1 cm the Planck-mean bolometric e missivity calculated for the pure beta-N-2 ice is 0.85. If the effecti ve N-2 grain size is 1 mm the emissivity is 0.40. Both are low enough to significantly affect surface energy balance calculations. The very narrow absorption features of alpha-N-2 result in even smaller bolomet ric emissivities of only 0.11 and 0.30 for 1 mm and 1 cm grain sizes a t 34 K. The effect of CH4 and CO, in solid solution with N-2 or as sep arate, intimately mixed grains, on the emissivity is also estimated. I t is found that the presence of either or both of these two molecules in solid solution with the N-2 ice on Triton and Pluto only slightly i ncreases the beta-N-2 emissivity. The emissivity of intimate mixtures of grains of CH4 and CO with N-2 is much less certain, and probably mu ch less applicable to Triton and Pluto. CH4 and CO in solid solution w ith alpha-N-2 increase the emissivity by about 50%. For an alpha-N-2 g rain size of 1 cm, the addition of 2% each CH4 and CO in solid solutio n with the N-2 increases the emissivity from 0.30 to 0.48 at 34 K. For a 1 mm grain size the emissivity of such a solid solution changes to 0.16 from 0.11. However, the emissivity of alpha-N-2 even with CH4 and /or CO in solution is still considerably lower than for beta-N-2. Seas onal variations on Triton and Pluto could be strongly influenced by th is emissivity contrast between the alpha and beta phases. In the extre me case of pure N-2 ice, Pluto's atmosphere could be prevented from fr eezing out, even at aphelion. Copyright (C) 1996 Elsevier Science Ltd