Nature 344, 315 - 317 (22 March 1990); doi:10.1038/344315a0

Dynamics of Triton's atmosphere

Andrew P. Ingersoll

Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125, USA

THE recent Voyager encounter established certain facts about Triton's atmosphere: the surface pressure is in the range 1.5–1.9 Pa (15–19 bar)¹; the surface temperature is 383K (ref. 2); molecular nitrogen is the dominant atmospheric constituent³; hazes and clouds are visible not only on the limb but also against the surface⁴; the wind in the southern hemisphere is to the northeast at low altitudes (as shown by streaks on the surface⁴) and to the west at high altitudes (as shown by geyser-like plume tails⁴). Triton rotates with a period of 5.877 days in a right-hand sense about the south pole, where the season now is late spring⁴. Here we argue that these features can be explained if Triton, like Mars⁵, has a global, well-structured atmosphere in equilibrium with surface frosts. The subliming frost cap produces a polar anticyclone at low altitudes, with northeastward winds of 5 m s^-1 within the Ekman boundary layer. The temperature contrast between the cold frost-covered pole and the warm unfrosted equator produces westward winds at high altitudes.

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