The thermal structure of Triton's atmosphere - Pre-Voyager models

Details The thermal structure of Triton's atmosphere - Pre-Voyager models The thermal structure of Triton's atmosphere - Pre-Voyager models

Aug 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989georl..16..973m&link_type=abstract

Geophysical Research Letters (ISSN 0094-8276), vol. 16, Aug. 1989, p. 973-976.

Physics

4

Atmospheric Models, Free Convection, Satellite Atmospheres, Triton, Brightness Temperature, Methane, Nitrogen, Optical Thickness, Rayleigh Scattering, Vapor Pressure, Neptune, Satellites, Triton, Hypotheses, Thermal Properties, Structure, Atmosphere, Models, Thickness, Composition, Nitrogen, Methane, Haze, Organic Material, Absorption, Opacity, Convection, Troposphere, Volatiles, Transport, Surface, Temperature, Stratosphere, Calculations, Pressure, Saturation, Depth

Scientific paper

Spectral data from earth observations have indicated the presence of N2 and CH4 on Triton. This paper outlines the use of the 1-D radiative-convective model developed for Titan to calculate the current pressure of N2 and CH4 on Triton. The production of haze material is obtained by scaling down from the Titan value. Results and predictions for the Voyager Triton encounter are as follows: A N2-CH4 atmosphere on Triton is thermodynamically self consistent and would have a surface pressure of approximately 50 millibar; due to the chemically produced haze, Triton has a hot atmosphere with a temperature of approximately 130 K; Triton's troposphere is a region of saturation of the major constituent of the atmosphere, N2.

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