The helium abundance of Jupiter from Voyager

@article{Gautier1980TheHA,
  title={The helium abundance of Jupiter from Voyager},
  author={Daniel Gautier and Barney J. Conrath and Michael Flasar and Rudolf A. Hanel and Virgil G. Kunde and Alain Ch{\'e}din and No{\"e}lle A. Scott},
  journal={Journal of Geophysical Research},
  year={1980},
  volume={86},
  pages={8713-8720}
}
The helium abundance in the Jovian atmosphere is derived from Voyager 1 data by two methods. The first method uses only infrared spectra from selected locations on the planet while the second method uses a thermal profile independently derived from radio occultation measurements and infrared spectra recorded near the occultation point. A hydrogen mole fraction of 0.897±0.030 is obtained from the first method, while the second method gives 0.880±0.036, corresponding to helium mass fractions of 0… 

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References

SHOWING 1-10 OF 43 REFERENCES

The Atmosphere of Jupiter: An Analysis of Voyager Radio Occultation Measurements.

Coherently related S (2.3 GHz) and X band (8.4 GHz) signals transmitted from Voyager 1 and 2 have been used to probe the Jovian atmosphere during occultations of the spacecraft by Jupiter. The

The abundance of helium in prominences and in the chromosphere

The abundance of helium relative to hydrogen is spectroscopically determined in prominences and in the chromosphere by using 1952, 1958, 1962 and 1966 eclipse data. Care is taken in the intensity

Albedo, internal heat, and energy balance of Jupiter: Preliminary results of the Voyager Infrared Investigation

Full disk measurements recorded 31 days before the Voyager 1 encounter with Jupiter by the radiometer (0.4–1.7 µm) of the infrared instrument Iris indicate a geometric albedo of 0.274±0.013. The

The Thermal Structure of Jupiter from Infrared Spectral Measurements by Means of a Filtered Iterative Inversion Method

Abstract The present study describes a filtering procedure to invert the radiative transfer equation which combines the advantages of the fast convergence of Chahine's method and the stability

Infrared Observations of the Jovian System from Voyager 1

The infrared spectroscopy and radiometry investigation has obtained spectra of Jupiter and its satellites between approximately 180 and 2500 cm–1 with a spectral resolution of 4.3 cm–1. The Jupiter

Helium abundance of the Sun

The solar abundance of helium (more specifically the ratio of solar helium to hydrogen) is a basic quantity in understanding many astrophysical and space physical problems. However, in spite of a

The Evidence for a Universal Helium and Deuterium Abundance

In view of the cosmological importance of early nucleosynthesis, a critical review has been made of the evidence for a lowest-level "universal" helium abundance. Except for high abundance (from

Radio Science with Voyager 1 at Jupiter: Preliminary Profiles of the Atmosphere and Ionosphere

Preliminary afternoon and predawn ionospheric profiles at 12� south latitude and near the equator have topside plasma scale heights changing to 960 kilometers above an altitucde of 3500 kilometers for the dayside, and about 960 kilomneters at all measured heights above the peak for the nightside.