Carbon Monoxide on Jupiter: Evidence for Both Internal and External Sources

Bézard, Bruno; Lellouch, E.; Strobel, D. F.; Maillard, J. P.; Drossart, P.

doi:10.1006/icar.2002.6917

Cited by 132 publications

(252 citation statements)

References 76 publications

(112 reference statements)

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“…It is unknown how much impactors have modified the composition of HD 209458b's atmosphere during its evolution. We note, however, that calculations by Bézard et al (2002) show that CO deposition by impactors cannot explain the observed abundance of CO ($1 part per billion, as opposed to essentially zero in equilibrium) in Jupiter's lower troposphere. On Jupiter, rather, disequilibrium results from convective upwelling from deep regions ( p $ 300 bars) where the equilibrium abundance of CO is higher.…”

Section: Introductionmentioning

confidence: 57%

“…It is related to pressure through the ideal gas equation of state. Using the proper eddy-mixing timescale derived by Smith (1998) for chemical quenching, Griffith & Yelle (1999) and Bézard et al (2002) demonstrate that the kinetic rates derived from the Yung et al (1988) reactions fit observations of CO in disequilibrium on the brown dwarf Gl 229b and on Jupiter. As noted above, the reaction proposed by Prinn & Barshay (1977) is too slow to account for the observed concentrations of CO in these objects.…”

Section: Chemical Pathways For Co Reductionmentioning

confidence: 85%

“…Using the updated reaction rate (eq. [8]) and the correct timescale for convective mixing, Bézard et al (2002) find that the reaction sequence for CO destruction suggested by Prinn & Barshay (1977) cannot explain the disequilibrium abundance of CO in Jupiter's troposphere. A faster reaction pathway for the reduction of CO to CH 4 must be sought.…”

Section: Chemical Pathways For Co Reductionmentioning

confidence: 98%

“…Bézard et al (2002) explore several explanations for the unexpected 1 part per billion CO concentration observed on this planet. They conclude that convective mixing from deeper layers remains the most likely source of Jupiter's tropospheric CO, although the reactions suggested by Prinn & Barshay (1977) are now thought to be too slow to explain the observed CO abundance.…”

Section: Chemical Pathways For Co Reductionmentioning

confidence: 99%

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Dynamics and Disequilibrium Carbon Chemistry in Hot Jupiter Atmospheres, with Application to HD 209458b

Cooper

Showman

2006

ApJ

238

340

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Chemical equilibrium considerations suggest that, assuming solar elemental abundances, carbon on HD 209458b is sequestered primarily as carbon monoxide (CO) and methane (CH 4 ). The relative mole fractions of CO(g) and CH 4 (g) in chemical equilibrium are expected to vary greatly according to variations in local temperature and pressure. We show, however, that in the p ¼ 1Y1000 mbar range, chemical equilibrium does not hold. To explore disequilibrium effects, we couple the chemical kinetics of CO and CH 4 to a three-dimensional numerical model of HD 209458b's atmospheric circulation. These simulations show that vigorous dynamics caused by uneven heating of this tidally locked planet homogenize the CO and CH 4 concentrations at p < 1 bar, even in the presence of lateral temperature variations of $500Y1000 K. In the 1Y1000 mbar pressure range we find that over 98% of the carbon is in CO. This is true even in cool regions where CH 4 is much more stable thermodynamically. Our work shows, furthermore, that planets 300Y500 K cooler than HD 209458b can also have abundant CO in their upper layers due to disequilibrium effects. We demonstrate several interesting observational consequences of these results. Subject headingg s: atmospheric effects -methods: numerical -planetary systemsplanets and satellites: general -planets and satellites: individual (HD 09458b)

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Section: Introductionmentioning

confidence: 57%

Section: Chemical Pathways For Co Reductionmentioning

confidence: 85%

Section: Chemical Pathways For Co Reductionmentioning

confidence: 98%

Section: Chemical Pathways For Co Reductionmentioning

confidence: 99%

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Dynamics and Disequilibrium Carbon Chemistry in Hot Jupiter Atmospheres, with Application to HD 209458b

Cooper

Showman

2006

ApJ

238

340

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“…One should note that Bézard et al (2002) had already demonstrated that Jupiter's CO vertical profile showed evidence for pre-SL9 comet impacts.…”

Section: Beyond Jupitermentioning

confidence: 99%

Constraints from Comets on the Formation and Volatile Acquisition of the Planets and Satellites

et al. 2015

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Comets play a dual role in understanding the formation and evolution of the solar system. First, the composition of comets provides information about the origin of the giant planets and their moons because comets formed early and their composition is not expected to have evolved significantly since formation. They, therefore serve as a record of conditions during the early stages of solar system formation. Once comets had formed, their orbits were perturbed allowing them to travel into the inner solar system and impact the planets. In this way they contributed to the volatile inventory of planetary atmospheres. We review here how knowledge of comet composition up to the time of the Rosetta mission has contributed to understanding the formation processes of the giant planets, their moons and small icy bodies in the solar system. We also discuss how comets contributed to the volatile inventories of the giant and terrestrial planets.

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