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Saturn Helium Abundance: A Reanalysis of Voyager Measurements
Thermal emission spectra calculated using Voyager Jupiter radio occultation (RSS) temperature profiles rescaled to the Galileo probe value of the helium abundance do not agree with the spectraExpand
The abundances of constituents of Titan's atmosphere from the GCMS instrument on the Huygens probe
Direct atmospheric measurements from the Gas Chromatograph Mass Spectrometer (GCMS), including altitude profiles of the constituents, isotopic ratios and trace species (including organic compounds), were reported, confirming the primary constituents were confirmed to be nitrogen and methane. Expand
Composition of Titan's lower atmosphere and simple surface volatiles as measured by the Cassini‐Huygens probe gas chromatograph mass spectrometer experiment
[1] The Cassini-Huygens probe gas chromatograph mass spectrometer (GCMS) determined the composition of the Titan atmosphere from ∼140 km altitude to the surface. After landing, it returnedExpand
Numerical simulation of the general circulation of the atmosphere of Titan.
Diagnostics of the simulated atmospheric circulation underlying the importance of the seasonal cycle and a tentative explanation for the creation and maintenance of the atmospheric superrotation based on a careful angular momentum budget are presented. Expand
Photochemical modeling of Titan's atmosphere
A new photochemical model of Titan's atmosphere which includes all the important compounds and reactions in spherical geometry from the surface to 1240 km is developed and is in a closer agreement with the abundances inferred from the Voyager infrared measurements at the equator than the Yung et al. results. Expand
The helium abundance of Saturn from Voyager measurements
Voyager radio-occultation and IR spectroscopy measurements are combined to infer an He mole fraction in the upper troposphere of Uranus of 0.152 + or - 0.033; the corresponding mass fraction is Y =Expand
Titan's atmosphere from Voyager infrared observations
Abstract We have studied the 900–1200 cm−1 range in three different selections of ∼30 Voyager 1 IRIS spectra recorded in Titan's equatorial region. In particular, we have reanalyzed the 8.6-μmExpand
Titan’s atmosphere from ISO mid-infrared spectroscopy
Abstract We have analyzed Titan observations performed by the Infrared Space Observatory (ISO) in the range 7–30 μm. The spectra obtained by three of the instruments on board the mission (the shortExpand
Titan's atmosphere and hypothesized ocean: A reanalysis of the Voyager 1 radio-occultation and IRIS 7.7-μm data
Voyager1 radio-occultation refractivity profiles of Titan in the 0–200 km altitude range are reanalyzed in order to derive limiting profiles for the equatorial thermal structure, taking into accountExpand
Infrared observations of the saturnian system from voyager 1.
During the passage of Voyager 1 through the Saturn system, the infrared instrument acquired spectral and radiometric data on Saturn, the rings, and Titan and other satellites, implying a depletion of helium in the atmosphere of Saturn relative to that of Jupiter. Expand