Structure of the Jovian Stratosphere at the Galileo Probe Entry Site

Yelle, R. V.; Griffith, C. A.; Young, L. A.

doi:10.1006/icar.2001.6640

Cited by 56 publications

(64 citation statements)

References 71 publications

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“…At cooler temperatures, TiO and VO condense and rain out, leaving Na and K as the main optical opacity sources, and allowing the radiation to penetrate to greater depths, with a behavior more like that of L dwarfs. Burrows et al (2008) find similar molecular behavior but also allow for absorption of additional hypothetical species, motivated by various tholins and photochemical species discussed in the context of solar system bodies (e.g., West et al 1986;Yelle et al 2001). Depending on where this postulated opacity source is placed, they find a variety of thermal inversions are possible.…”

Section: Discussionmentioning

confidence: 99%

On the Absorption and Redistribution of Energy in Irradiated Planets

Hansen

2008

Astrophysical Journal Supplement Series, The

140

148

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We present a sequence of toy models for irradiated planet atmospheres, in which the effects of geometry and energy redistribution are modeled self-consistently. We use separate but coupled gray atmosphere models to treat the ingoing stellar irradiation and outgoing planetary reradiation. We investigate how observed quantities such as full phase secondary eclipses and orbital phase curves depend on various important parameters, such as the depth at which irradiation is absorbed, the depth at which energy is redistributed, and the eccentricity of the orbit. We also compare our results to the more detailed radiative transfer models in the literature in order to understand how those map onto the toy model parameter space. Such an approach can prove complementary to more detailed calculations, in that they demonstrate, in a simple way, how the solutions change depending on where, and how, energy redistribution occurs. As an example of the value of such models, we demonstrate how energy redistribution and temperature equilibration at moderate optical depths can lead to temperature inversions in the planetary atmosphere, which is of some relevance to recent observational findings.

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Section: Discussionmentioning

confidence: 99%

On the Absorption and Redistribution of Energy in Irradiated Planets

Hansen

2008

Astrophysical Journal Supplement Series, The

140

148

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“…Sada et al (1998) measured a mole fraction of acetylene of (1.8 -2.8) ϫ 10 Ϫ8 in the 1-to 40-mbar region while Noll et al (1986) measured a mixing ratio of (0.7-1.3) ϫ 10 Ϫ7 at about 1.5 mbar. Higher altitude measurements, by Yelle et al (2001) and Bézard et al (1997), yielded respectively a mole fraction of (2-3) ϫ 10 Ϫ6 from 0.004 to 0.02 mbar and a mixing ratio of 1 ϫ 10…”

Section: ϫ8mentioning

confidence: 99%

“…This calculation assumes the C 2 H 2 distribution of model D for pressures higher than 20 mbar. At lower pressures, a distribution simultaneously consistent with the 0-to 20-mbar column abundance of model D and with the results from Noll et al (1986), Sada et al (1998), and Yelle et al (2001) is adopted. This calculation also assumes a thermal profile formed from a smoothed Galileo/ASI profile at pressures lower than 0.1 bar (Yelle et al, 2001) and a thermal profile from the SEB for pressures greater than 0.1 bar [derived following the techniques of Griffith et al (1992)].…”

Section: ϫ7mentioning

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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“…Changes in insolation with latitude over a saturnian year cause latitudinal variations of temperature and photochemistry. Saturn's stratosphere is very similar to Jupiter's, where it has recently been shown that C 2 H 2 and C 2 H 6 are the dominant coolants (Yelle et al, 2001). These molecules are photochemical byproducts of methane photolysis, so their abundance versus latitude may be tied to seasonally varying insolation.…”

Section: Introductionmentioning

confidence: 97%