Benzene on the Giant Planets*1

Bézard, Bruno

doi:10.1006/icar.2001.6719

Cited by 81 publications

(63 citation statements)

References 18 publications

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“…In the lower stratosphere, the profile appears to be 8 K warmer between 0.05 and 1 mbar, and 3 K colder below the 20 mbar level, than the disk-averaged profile proposed by Bézard et al (1999Bézard et al ( , 2000 to interpret ISO detections of the CH 3 radical and C 6 H 6 on Neptune. Finally, we note that our modeling applies well for regions into the upper stratosphere (i.e.…”

Section: Discussionmentioning

confidence: 58%

Improved constraints on Neptune's atmosphere from submillimetre-wavelength observations

Marten¹,

Matthews

Owen

et al. 2005

A&A

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Abstract. We describe observations of Neptune carried out using the James Clerk Maxwell Telescope (Mauna Kea, Hawaii) during September 1998. High-quality data for the sub-mm-wavelength rotational transitions of HCN (J = 4−3) and CO (J = 3−2 and 4−3) were obtained, and we use the data to make improved determinations of the abundances of these trace species and the temperature profile of Neptune's atmosphere.

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Section: Discussionmentioning

confidence: 58%

Improved constraints on Neptune's atmosphere from submillimetre-wavelength observations

Marten¹,

Matthews

Owen

et al. 2005

A&A

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“…This conclusion rests on the assumption of homogenous benzene concentration through the stratosphere. Bézard et al (2001) suggested that the ion-related chemistry proposed by Wong et al (2000) was probably inadequate to explain the observed C 6 H 6 abundance at midlatitudes. Spatially resolved astronomical observations of benzene, as a tracer of PAH production, could be very helpful in this regard.…”

Section: Implications For Haze Formation In the Stratosphere Of Jupitermentioning

confidence: 99%

“…As on Titan (Wilson & Atreya 2003;Wong et al 2003), polyyne polymerization (C 2n+2 H 2 , n ≥ 1) initiated with the photodissociation of acetylene, creating the ethynyl radical (C 2 H) through hydrogen abstraction, was also considered, as well as HCN polymerization . The detection by the Voyager Infrared Interferometer Spectrometer (IRIS) of the first ring compound, benzene (C 6 H 6 ), in the north polar region (Kim et al 1985) and the recent observation of significant amounts of benzene at mid latitudes in the upper atmosphere by the Infrared Space Observatory (Bézard et al 2001) promote a scenario in which aromatics play a key role in haze formation.…”

Section: Introductionmentioning

confidence: 99%

Insights into the role of polycyclic aromatic hydrocarbon condensation in haze formation in Jupiter’s atmosphere

Biennier

Sabbah

Chandrasekaran

et al. 2011

A&A

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Context. The haze in the atmosphere of Jupiter has been proposed to originate mostly from the condensation of low mass PAHs. Under this hypothesis, the transition of gas phase molecular species to solid particles is achieved by the formation of a critical nucleus composed of two small PAH molecules held together by van der Waals forces. Aims. Laboratory experiments coupled with theoretical calculations explore the thermodynamics and kinetics of PAH dimerization with the objective to assess this pathway in the production of nuclei of haze particles. Methods. We have performed experiments to identify the temperature range over which small PAH clusters form in supersaturated uniform supersonic flows. The kinetics of this formation has also been investigated. The chemical species present in the reactor are probed by a time-of-flight mass spectrometer equipped with a VUV laser for photoionisation of the neutral reagents and products. The experimental data were combined with theoretical calculations that employ careful consideration of the intermolecular interaction energies and intermolecular dynamics to estimate the binding energy, equilibrium constant, and rate constant. Results. We found that low-mass PAHs such as anthracene (C 14 H 10 ) and pyrene (C 16 H 10 ) can not homogeneously nucleate in the upper stratosphere at the altitude at which haze formation has been proposed to commence. Other chemical or physical processes should be considered to account for aerosol nuclei formation.

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“…In parallel, the benzene (C 6 H 6 ) column density has been measured in the stratospheres of Jupiter and Saturn (disk average) using the Infrared Space Observatory (Bézard et al 2001). In the case of Jupiter's polar atmosphere, benzene has been proposed as a precursor to the formation of more complex hydrocarbons, such as polyacetylenes and multi-ring compounds, which could condense to form polar aerosols (Wong et al 2000(Wong et al , 2003Friedson et al 2002).…”

Section: Introductionmentioning

confidence: 99%

Stratospheric benzene and hydrocarbon aerosols detected in Saturn’s auroral regions

Guerlet

Fouchet

Vinatier

et al. 2015

A&A

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Context. Saturn's polar upper atmosphere exhibits significant auroral activity; however, its impact on stratospheric chemistry (i.e. the production of benzene and heavier hydrocarbons) and thermal structure remains poorly documented. Aims. We aim to bring new constraints on the benzene distribution in Saturn's stratosphere, to characterize polar aerosols (their vertical distribution, composition, thermal infrared optical properties), and to quantify the aerosols' radiative impact on the thermal structure. Methods. Infrared spectra acquired by the Composite Infrared Spectrometer (CIRS) on board Cassini in limb viewing geometry are analysed to derive benzene column abundances and aerosol opacity profiles over the 3 to 0.1 mbar pressure range. The spectral dependency of the haze opacity is assessed in the ranges 680-900 and 1360-1440 cm −1 . Then, a radiative climate model is used to compute equilibrium temperature profiles, with and without haze, given the haze properties derived from CIRS measurements. Results. On Saturn's auroral region (80• S), benzene is found to be slightly enhanced compared to its equatorial and mid-latitude values. This contrasts with the Moses & Greathouse (2005, J. Geophys. Res., 110, 9007) photochemical model, which predicts a benzene abundance 50 times lower at 80• S than at the equator. This advocates for the inclusion of ion-related reactions in Saturn's chemical models. The polar stratosphere is also enriched in aerosols, with spectral signatures consistent with vibration modes assigned to aromatic and aliphatic hydrocarbons, and presenting similarities with the signatures observed in Titan's stratosphere. The aerosol mass loading at 80• S is estimated to be 1−4 × 10 −5 g cm −2 , an order of magnitude less than on Jupiter, which is consistent with the order of magnitude weaker auroral power at Saturn. We estimate that this polar haze warms the middle stratosphere by 6 K in summer and cools the upper stratosphere by 5 K in winter. Hence, aerosols linked with auroral activity can partly account for the warm polar hood observed in Saturn's summer stratosphere.

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Benzene on the Giant Planets*1

Cited by 81 publications

References 18 publications

Improved constraints on Neptune's atmosphere from submillimetre-wavelength observations

Improved constraints on Neptune's atmosphere from submillimetre-wavelength observations

Insights into the role of polycyclic aromatic hydrocarbon condensation in haze formation in Jupiter’s atmosphere

Stratospheric benzene and hydrocarbon aerosols detected in Saturn’s auroral regions

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