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Triton: Scattering models and surface/atmosphere constraints
Author(s) -
Thompson W. Reid
Publication year - 1989
Publication title -
geophysical research letters
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.007
H-Index - 273
eISSN - 1944-8007
pISSN - 0094-8276
DOI - 10.1029/gl016i008p00969
Subject(s) - opacity , geometric albedo , haze , scattering , atmosphere (unit) , infrared , absorption (acoustics) , radius , diffuse sky radiation , albedo (alchemy) , optics , materials science , physics , astrophysics , photometry (optics) , meteorology , stars , art , computer security , performance art , computer science , art history
Modeling of Triton's spectrum indicates a bright scattering layer of optical depth τ ≃ 3 overlying an optically deep layer of CH 4 with high absorption and little scattering. UV absorption in the spectrum indicates τ ≃ 0.3 of red‐yellow haze, although some color may also arise from complex organics partially visible on the surface. An analysis of this and other (spectro) photometric evidence indicates that Triton most likely has a bright surface, which was partially visible in 1977–1980. Geometric albedo p = 0.62 −0.12 +0.18 , radius r = 1480 ± 180km, and temperature T = 48 ± 6 K. With scattering optical depths of 0.3–3 and ∼ 1–10mb of N 2 , a Mars‐like atmospheric density and surface visibility pertain. Imaging with the 0.62 µm CH 4 filter of the Voyager 2 wide angle camera could show ∼20% contrast between the average surface and clean exposures of CH 4 ice (which is not limited to the polar caps). Low far‐infrared atmospheric opacity will in principle allow the detection of thermal gradients in the surface caused by optically transmitting but infrared opaque CH 4 and N 2 ice.