The C/H ratio in Jupiter from the Voyager infrared investigation

Gautier, D.; Bézard, Bruno; Marten, A.; Baluteau, J. P.; Scott, Nicholas J.; Chédin, A.; Kunde, V. G.; Hanel, Reinhold

doi:10.1086/160040

Cited by 84 publications

(18 citation statements)

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“…For example, to produce an approximately 2 K offset in brightness temperature at 350 cm −1 , an error of 1 K in the instrument temperature would be required, and this same error would result in a brightness temperature error greater than 6 K at 600 cm −1 . Finally, we note that the C/H ratio in Jupiter obtained using a thermal profile directly retrieved from the IRIS spectra (Gautier et al 1982), rather than using an RSS profile, is quite close to that measured in situ by the Galileo probe (Niemann et al 1996(Niemann et al , 1998. From these considerations, it seems unlikely that errors in the IRIS absolute calibration could account for the differences observed in Fig.…”

Section: Figsupporting

confidence: 70%

Saturn Helium Abundance: A Reanalysis of Voyager Measurements

Conrath

Gautier

2000

Icarus

205

160

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Section: Figsupporting

confidence: 70%

Saturn Helium Abundance: A Reanalysis of Voyager Measurements

Conrath

Gautier

2000

Icarus

205

160

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“…This stems from the fact that Jupiter's CH 4 tropospheric abundance is well known, especially after the Galileo Probe measurements (Niemann et al 1998) which confirmed the Voyager 1 spectroscopic determination (Gautier et al 1982).…”

Section: Jupitermentioning

confidence: 72%

The deuterium abundance in Jupiter and Saturn from ISO-SWS observations

Lellouch

Bézard

Fouchet

et al. 2001

A&A

218

157

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Abstract.Observations with the Short Wavelength Spectrometer (SWS) onboard the Infrared Space Observatory (ISO) are used to determine the D/H ratio in Jupiter's and Saturn's atmospheres. The D/H ratio is measured independently in hydrogen (i.e. from the HD/H2 ratio) and methane (from CH3D/CH4). Observations of the HD R(2) and R(3) rotational lines at 37.7 and 28.5 µm, of the H2 S(0) and S(1) quadrupolar lines at 17.1 and 28.2 µm, of the methane ν4 band at 7.7 µm, and of the CH3D ν6 band at 8.6 µm are analyzed jointly, allowing a retrieval of thermal profiles and molecular abundances.

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“…Least squares fits of measured absorption in the Q branch region and the R(8) manifold were made with the model and data described above. The choice of the particular R(8) manifold results from three reasons; the first is that the R branch is more adapted for the determination of A(R,R)ϭA( P, P); indeed, 3 lines within the manifolds are more closely spaced and less contaminated by transitions of other bands in the R branch than in the P branch. The second point is that important line-mixing effects ͑and thus high sensitivity to A͒ occur for high rotational quantum numbers.…”

Section: Data Usedmentioning

confidence: 99%

Experimental and theoretical study of line mixing in methane spectra. I. The N2-broadened ν3 band at room temperature

Pieroni

Nguyen‐Van‐Thanh

Brodbeck

et al. 1999

The Journal of Chemical Physics

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Line-mixing effects have been studied in the 3 band of CH 4 perturbed by N 2 at room temperature. New measurements have been made and a model is proposed which is not, for the first time, strictly empirical. Three different experimental set ups have been used in order to measure absorption in the 2800-3200 cm Ϫ1 spectral region for total pressures in the 0.25-2 and 25-80 atm ranges. Analysis of the spectra demonstrates the significant influence of line mixing on the shape of the Q branch and of the P and R manifolds. A model is proposed which is based on state-to-state collisional transfer rates calculated from the intermolecular potential surface with a semiclassical approach. The line-coupling relaxation matrix is constructed from these data and two additional parameters which are fitted on measured absorption. Comparisons between measurements and spectra computed accounting for and neglecting line mixing are made. They prove the quality of the approach which satisfactory accounts for the effects of pressure and of rotational quantum numbers on the spectral shape under conditions where modifications introduced by line mixing are important. For high rotational quantum number lines, the main features induced by collisions are predicted but some discrepancies remain; the latter may be due to improper line-coupling elements but there is strong evidence that the use of inaccurate line broadening parameters also contributes to errors in calculated spectra.

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The C/H ratio in Jupiter from the Voyager infrared investigation

Cited by 84 publications

References 0 publications

Saturn Helium Abundance: A Reanalysis of Voyager Measurements

Saturn Helium Abundance: A Reanalysis of Voyager Measurements

The deuterium abundance in Jupiter and Saturn from ISO-SWS observations

Experimental and theoretical study of line mixing in methane spectra. I. The N2-broadened ν3 band at room temperature

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