Titan trace gaseous composition from CIRS at the end of the Cassini–Huygens prime mission

Coustenis, A.; Jennings, Donald E.; Nixon, C. A.; Achterberg, R. K.; Lavvas, P.; Vinatier, S.; Teanby, N. A.; Bjoraker, G. L.; Carlson, R.; Piani, Laurette; Bampasidis, G.; Flasar, F. M.; Romani, P. N.

doi:10.1016/j.icarus.2009.11.027

Cited by 168 publications

(115 citation statements)

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“…Latitudinal variations in Titan's stratospheric thermal and chemical structure have been reported in the past from Cassini data acquired by the Composite Infrared Spectrometer (CIRS) (Flasar et al 2005;Teanby et al 2006;Coustenis et al 2007Coustenis et al , 2008Coustenis et al , 2010de Kok et al 2007;Teanby et al , 2008Teanby et al , 2009aVinatier et al 2007Vinatier et al , 2010Nixon et al 2008a;Achterberg et al 2008Achterberg et al , 2011. Here, we explore the thermal and chemical evolution discernible within the timeframe from 2006 to 2012, thus complementing and refining previous reports from earlier stages of the mission.…”

Section: Context and Observationsmentioning

confidence: 56%

“…The Cassini/CIRS spectra are analyzed using a method extensively described in previous articles (Coustenis et al 2007(Coustenis et al , 2010. In brief, we model Titan's thermal infrared spectrum by use of a line-by-line monochromatic radiative transfer code updated from the one we used in previous Titan atmospheric structure retrievals (Coustenis et al 2010, and references therein).…”

Section: Discussionmentioning

confidence: 99%

“…In brief, we model Titan's thermal infrared spectrum by use of a line-by-line monochromatic radiative transfer code updated from the one we used in previous Titan atmospheric structure retrievals (Coustenis et al 2010, and references therein). In this new release (ARTT, for Atmospheric Radiative Transfer for Titan), we have included more constituents relevant to Titan's chemistry (26 species in total, all the so-far detected hydrocarbons, nitriles, and oxygen compounds in addition to the main molecules N 2 , H 2 , CH 4, and argon).…”

Section: Discussionmentioning

confidence: 99%

“…As explained in detail in Section 4.4 of Coustenis et al (2010), the use of constant vertical profiles does not allow for a good fit of the whole C 2 H 2 emission band centered at 729 cm −1 . We therefore first derive the C 2 H 2 abundance that fits the Q-branch and then adjust the fit in the wings of the band to infer the other mixing ratios of the weaker species in the 620-780 cm −1 region.…”

Section: Discussionmentioning

confidence: 99%

“…The average signal-to-noise ratio is shown as well as the corresponding Cassini Titan flyby(s) and the relative solar longitude (Ls). The selections we made in order to enhance the signal-to-noise ratio cover different latitudes on Titan (we sum all longitudes because no longitudinal variations were found in our studies; Coustenis et al 2007Coustenis et al , 2010. The averaged spectra created from the highresolution nadir data in the several latitudinal bins (between 50 • S and 50 • N) contain a large number of spectra in general, with some exceptions (as indicated in Tables 1-4).…”

Section: Context and Observationsmentioning

confidence: 99%

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THERMAL AND CHEMICAL STRUCTURE VARIATIONS IN TITAN'S STRATOSPHERE DURING THECASSINIMISSION

Bampasidis

Coustenis

Achterberg

et al. 2012

ApJ

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We have developed a line-by-line Atmospheric Radiative Transfer for Titan code that includes the most recent laboratory spectroscopic data and haze descriptions relative to Titan's stratosphere. We use this code to model Cassini Composite Infrared Spectrometer data taken during the numerous Titan flybys from 2006 to 2012 at surface-intercepting geometry in the 600-1500 cm −1 range for latitudes from 50 • S to 50 • N. We report variations in temperature and chemical composition in the stratosphere during the Cassini mission, before and after the Northern Spring Equinox (NSE). We find indication for a weakening of the temperature gradient with warming of the stratosphere and cooling of the lower mesosphere. In addition, we infer precise concentrations for the trace gases and their main isotopologues and find that the chemical composition in Titan's stratosphere varies significantly with latitude during the 6 years investigated here, with increased mixing ratios toward the northern latitudes. In particular, we monitor and quantify the amplitude of a maximum enhancement of several gases observed at northern latitudes up to 50 • N around mid-2009, at the time of the NSE. We find that this rise is followed by a rapid decrease in chemical inventory in 2010 probably due to a weakening north polar vortex with reduced lateral mixing across the vortex boundary.

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Section: Context and Observationsmentioning

confidence: 56%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Context and Observationsmentioning

confidence: 99%

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THERMAL AND CHEMICAL STRUCTURE VARIATIONS IN TITAN'S STRATOSPHERE DURING THECASSINIMISSION

Bampasidis

Coustenis

Achterberg

et al. 2012

ApJ

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Dissolution on Titan and on Earth: Toward the age of Titan's karstic landscapes

et al. 2015

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Titan's polar surface is dotted with hundreds of lacustrine depressions. Based on the hypothesis that they are karstic in origin, we aim at determining the efficiency of surface dissolution as a landshaping process on Titan, in a comparative planetology perspective with the Earth as reference. Our approach is based on the calculation of solutional denudation rates and allow inference of formation timescales for topographic depressions developed by chemical erosion on both planetary bodies. The model depends on the solubility of solids in liquids, the density of solids and liquids, and the average annual net rainfall rates. We compute and compare the denudation rates of pure solid organics in liquid hydrocarbons and of minerals in liquid water over Titan and Earth timescales. We then investigate the denudation rates of a superficial organic layer in liquid methane over one Titan year. At this timescale, such a layer on Titan would behave like salts or carbonates on Earth depending on its composition, which means that dissolution processes would likely occur, but would be 30 times slower on Titan compared to the Earth due to the seasonality of precipitation. Assuming an average depth of 100 m for Titan's lacustrine depressions, these could have developed in a few tens of millions of years at polar latitudes higher than 70 • N and S, and a few hundreds of million years at lower polar latitudes. The ages determined are consistent with the youth of the surface (< 1 Gyr) and the repartition of dissolution-related landforms on Titan.

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Titan's atmosphere and climate

2017

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Titan is the only moon with a substantial atmosphere, the only other thick N2 atmosphere besides Earth's, the site of extraordinarily complex atmospheric chemistry that far surpasses any other solar system atmosphere, and the only other solar system body with stable liquid currently on its surface. The connection between Titan's surface and atmosphere is also unique in our solar system; atmospheric chemistry produces materials that are deposited on the surface and subsequently altered by surface‐atmosphere interactions such as aeolian and fluvial processes resulting in the formation of extensive dune fields and expansive lakes and seas. Titan's atmosphere is favorable for organic haze formation, which combined with the presence of some oxygen‐bearing molecules indicates that Titan's atmosphere may produce molecules of prebiotic interest. The combination of organics and liquid, in the form of water in a subsurface ocean and methane/ethane in the surface lakes and seas, means that Titan may be the ideal place in the solar system to test ideas about habitability, prebiotic chemistry, and the ubiquity and diversity of life in the universe. The Cassini‐Huygens mission to the Saturn system has provided a wealth of new information allowing for study of Titan as a complex system. Here I review our current understanding of Titan's atmosphere and climate forged from the powerful combination of Earth‐based observations, remote sensing and in situ spacecraft measurements, laboratory experiments, and models. I conclude with some of our remaining unanswered questions as the incredible era of exploration with Cassini‐Huygens comes to an end.

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Titan trace gaseous composition from CIRS at the end of the Cassini–Huygens prime mission

Cited by 168 publications

References 37 publications

THERMAL AND CHEMICAL STRUCTURE VARIATIONS IN TITAN'S STRATOSPHERE DURING THECASSINIMISSION

THERMAL AND CHEMICAL STRUCTURE VARIATIONS IN TITAN'S STRATOSPHERE DURING THECASSINIMISSION

Dissolution on Titan and on Earth: Toward the age of Titan's karstic landscapes

Titan's atmosphere and climate

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