May 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984icar...58..293c&link_type=abstract
(IAU, COSPAR, NASA, et al., Colloquium on Natural Satellites, 77th, Cornell University, Ithaca, NY, July 5-9, 1983) Icarus (ISSN
Other
80
Abundance, Infrared Absorption, Infrared Spectra, Liquid Nitrogen, Satellite Surfaces, Triton, Ice, Methane, Photochemical Reactions, Satellite Atmospheres, Solidified Gases, Surface Temperature, Neptune, Satellites, Triton, Nitrogen, Infrared, Spectra, Absorption, Observations, Calculations, Abundance, Depth, Surface, Comparisons, Saturn, Titan, Models, Liquids, Methane, Composition, Photochemistry, Radiometry, Size, Radius, Albedo, Atmosphere, Vapor Pressure, Data, Temperature, Chemistry, Diameter, Physic
Scientific paper
The near-infrared spectrum of Triton is characterized by strong absorption bands of methane, probably in the solid state. An additional absorption band at 2.16 μm is tentatively identified as the density-induced (2-0) band of molecular nitrogen in the liquid state. Using the absorption coefficient for this band derived from laboratory observations and from the literature, it is calculated that Triton must have a layer of nitrogen at least tens of centimeters deep over much of its surface. The Triton spectrum has been modeled with liquid nitrogen and solid methane, and it is found that the shape of the continuum in two spectral regions can be properly accounted for by adding a spectral component corresponding to fine-grained water frost. It is speculated that yet another component, a dark, solid, photochemical derivative of methane, may occur as a trace contaminant of the surface materials. If much of the surface of Triton is liquid, the radiometric observations of the satellite must be reinterpreted to derive the radius and surface albedo.
Brown Harvey R.
Clark Roger Nelson
Cruikshank Dale P.
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