Study of the Ammonia ice cloud layer in the equatorial region of Jupiter from the infrared interferometric experiment on voyager

Marten, A.; Rouan, D.; Baluteau, J. P.; Gautier, D.; Conrath, B. J.; Hanel, Rudolf; Kunde, V. G.; Samuelson, R. E.; Chédin, A.; Scott, N. A.

doi:10.1016/0019-1035(81)90211-6

Cited by 64 publications

(16 citation statements)

References 18 publications

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“…Brooke et al (1998) have modeled this part of the Jupiter spectrum including multiple scattering by spherical cloud particles, and have obtained a good ®t of the data with a two-cloud model including NH 3 ice particles of about 10 mm size in the upper cloud near 0.55 bar. These results agree reasonably well with previous work by Marten et al (1981), Orton et al (1982), West et al (1986) and Gierasch et al (1986); they differ, in contrast with the conclusions derived from Carlson et al (1993Carlson et al ( , 1994 and from Irwin et al (1998). Carlson et al (1993Carlson et al ( , 1994) favored a bimodal (3 mm, 100 mm) distribution of particles based on the absence of NH 3 ice resonant absorption features in Voyager IRIS spectra (5±50 mm) and the comparison of 5 and 50 mm radiances.…”

Section: The Iso Spectrasupporting

confidence: 87%

The atmospheric composition and structure of Jupiter and Saturn from ISO observations: a preliminary review

Encrenaz

Drossart

Feuchtgruber

et al. 1999

Planetary and Space Science

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Section: The Iso Spectrasupporting

confidence: 87%

The atmospheric composition and structure of Jupiter and Saturn from ISO observations: a preliminary review

Encrenaz

Drossart

Feuchtgruber

et al. 1999

Planetary and Space Science

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“…Infrared observations of NH 3 (Tokunaga et al, 1980;Marten et al, 1981;Kunde et al, 1982;Gierasch et al, 1986;Lellouch et al, 1989;Griffith et al, 1992;Carlson et al, 1993Carlson et al, , 1994Encrenaz et al, 1996;Lara et al, 1998) of predominantly the North Equatorial Belt (NEB), the North Tropical Zone (NTZ), the South Tropical Zone (STZ) and the Great Red Spot (GRS) are consistent with theoretical predictions. Near solar or greater abundances of nitrogen, locked in ammonia, at pressures greater than 1 bar have been detected.…”

Section: ϫ8supporting

confidence: 54%

“…IRIS spectra suffer from low signal-to-noise ratios. Marten et al (1981), Kunde et al (1982), Gierasch et al (1986), Griffith et al (1992), and Carlson et al (1993Carlson et al ( , 1994 averaged together many spectra, over all longitudes within small latitudinal bands and from 0 to 30°in emission angles, to improve the signal-to-noise. More recent observations looked at a larger fraction of the jovian atmosphere simultaneously.…”

Section: Interpretation Of Spectrum and Discussionmentioning

confidence: 99%

HST observation of the atmospheric composition of Jupiter’s equatorial region: evidence for tropospheric C2H2☆

Bétrémieux

Yelle

Griffith

2003

Icarus

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This paper presents the first detailed analysis of acetylene absorption features observed longward of 190.0 nm in a jovian spectrum by the Faint Object Spectrograph on board the Hubble Space Telescope. The presence of two features located near 207.0 nm can only be explained by a substantial abundance of acetylene in the upper troposphere. Using a Rayleigh-Raman radiative transfer model, it was determined that the acetylene vertical profile is characterized by a decrease in the mole fraction with increasing pressure in the upper stratosphere, a minimum around 14 to 29 mbar, followed by an increase to about 1.5 ϫ 10 Ϫ7 in the upper troposphere. Longward of 220 nm, the relatively high contrast of Raman features to the continuum precludes the existence of an optically significant amount of clouds from 150 to 500 mbar unless they are highly reflective. Instead, the reflectivity at these long wavelengths is determined by stratospheric, not tropospheric, scatterers and absorbers. Analysis of the data also suggests that ammonia is extremely undersaturated at pressures below 700 mbar. However, no firm conclusions can be reached because of the uncertainties surrounding its cross section longward of 217.0 nm, which are due to vibrationally excited states.

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“…For example, a spectrum from the 23.51N region is well matched by the synthetic spectrum including a cloud of ammonia ice particles near 1 mm in size, with a total optical depth of 0.75, while a spectrum from 151N does not exhibit the ammonia ice feature. The particles detected via this 10-mm ammonia ice feature are smaller than the 2-30 mm ammonia ice particles invoked to fit the Jovian spectra at 3 mm by Brooke et al (1998) and Baines et al (2002), and at 10 mm by Marten et al (1981), Orton et al (1982), and Shaffer et al (1986).…”

Section: Galileo Nims and Cassini Cirs Observations Of Siacmentioning

confidence: 67%

Jupiter's ammonia clouds—localized or ubiquitous?

Atreya

Wong

Baines

et al. 2005

Planetary and Space Science

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From an analysis of the Galileo Near Infrared Imaging Spectrometer (NIMS) data, Baines et al. (Icarus 159 (2002) 74) have reported that spectrally identifiable ammonia clouds (SIACs) cover less than 1% of Jupiter. Localized ammonia clouds have been identified also in the Cassini Composite Infrared Spectrometer (CIRS) observations (Planet. Space Sci. 52 (2004a) 385). Yet, groundbased, satellite and spacecraft observations show that clouds exist everywhere on Jupiter. Thermochemical models also predict that Jupiter must be covered with clouds, with the top layer made up of ammonia ice. For a solar composition atmosphere, models predict the base of the ammonia clouds to be at 720 mb, at 1000 mb if N/H were 4 Â solar, and at 0.5 bar for depleted ammonia of 10 À2 Â solar (Planet. Space Sci. 47 (1999) 1243). Thus, the above NIMS and CIRS findings are seemingly at odds with other observations and cloud physics models. We suggest that the clouds of ammonia ice are ubiquitous on Jupiter, but that spectral identification of all but the freshest of the ammonia clouds and high altitude ammonia haze is inhibited by a combination of (i) dusting, starting with hydrocarbon haze particles falling from Jupiter's stratosphere and combining with an even much larger source-the hydrazine haze; (ii) cloud properties, including ammonia aerosol particle size effects. In this paper, we investigate the role of photochemical haze and find that a substantial amount of haze material can deposit on the upper cloud layer of Jupiter, possibly enough to mask its spectral signature. The stratospheric haze particles result from condensation of polycyclic aromatic hydrocarbons (PAHs), whereas hydrazine ice is formed from ammonia photochemistry. We anticipate similar conditions to prevail on Saturn. r

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Study of the Ammonia ice cloud layer in the equatorial region of Jupiter from the infrared interferometric experiment on voyager

Cited by 64 publications

References 18 publications

The atmospheric composition and structure of Jupiter and Saturn from ISO observations: a preliminary review

The atmospheric composition and structure of Jupiter and Saturn from ISO observations: a preliminary review

HST observation of the atmospheric composition of Jupiter’s equatorial region: evidence for tropospheric C2H2☆

Jupiter's ammonia clouds—localized or ubiquitous?

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