Particle size and abundance of HC3N ice in Titan’s lower stratosphere at high northern latitudes

Anderson, C. M.; Samuelson, R. E.; Bjoraker, G. L.; Achterberg, R. K.

doi:10.1016/j.icarus.2009.12.024

Cited by 48 publications

(49 citation statements)

References 30 publications

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“…in Voyager IRIS and Cassini CIRS spectra at far-and mid-infrared wavelengths (Samuelson et al, 1997;Coustenis et al, 1999;Khanna, 2005;Samuelson et al, 2007;Anderson et al, 2010). In the spectra, the condensate features are typically broader than those associated with trace gas emission.…”

Section: Discussionmentioning

confidence: 99%

The structure of Titan’s atmosphere from Cassini radio occultations: Occultations from the Prime and Equinox missions

Schinder

Flasar

Marouf

et al. 2012

Icarus

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Section: Discussionmentioning

confidence: 99%

The structure of Titan’s atmosphere from Cassini radio occultations: Occultations from the Prime and Equinox missions

Schinder

Flasar

Marouf

et al. 2012

Icarus

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“…1r uncertainties can range from about 2 K at low latitudes to as much as 10 K at very cold high northern latitudes, where the lines are especially weak (see Anderson et al, 2010).…”

Section: Temperature Structure At 15°n 15°s and 55°smentioning

confidence: 99%

Titan’s aerosol and stratospheric ice opacities between 18 and 500μm: Vertical and spectral characteristics from Cassini CIRS

Anderson

Samuelson

2011

Icarus

112

118

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“…The next step in Titan's chemical evolution knowledge is the fate of the aerosols once they reach to the surface. Strong evidence for the nitrile ice feature due to HCN, HC 3 N, and C 4 N 2 exists (Samuelson et al 1997;Anderson et al 2010;Khanna et al 1987;de Kok et al 2014). We have recently shown that in the condensed-phase molecules such as C 4 N 2 can be photochemically polymerized at longer wavelength photons that penetrate through into the lower atmosphere of Titan (Gudipati et al 2013;Couturier-Tamburelli et al 2014a).…”

Section: Introductionmentioning

confidence: 99%

Simulation of Titan’s atmospheric photochemistry

Couturier-Tamburelli

Piétri

Gudipati

2015

A&A

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We studied the photochemistry of frozen ice of a polar Titan's atmospheric molecule cyanodiacetylene (HC 5 N) to determine the possible contribution of this compound to the lower altitude photochemistry of haze layers found on Titan. We used infrared analysis to examine the residue produced by irradiation of solid HC 5 N at λ > 300 nm. The resulting polymer is orange-brown in color. Based on theoretical analysis and the general tendency of HC 5 N and C 4 N 2 to undergo similar ice photochemistry at longer wavelengths accessible in Titan's lower atmosphere, we conclude that Titan's lower atmosphere is photochemically active in the regions of cloud, ice, and aerosol formation. C 4 N 2 is a symmetric molecule with no net dipole moment whereas, HC 5 N has a large dipole moment of ∼4 D. Consequently, though both these molecules have very similar molecular weight and size, their sublimation temperatures are different, HC 5 N subliming around 170 K compared to 160 K for C 4 N 2 . Based on our studies we conclude that in Titan's atmosphere the cyanoacetylene class of molecules (HCN, HC 3 N, HC 5 N, etc.) would condense first followed by the dicyanoacetylenes (C 2 N 2 , C 4 N 2 , C 6 N 2 , etc.), leading to fractionation of different class of molecules. From the fluxes used in the laboratory and depletion of the original HC 5 N signals, we estimate Titan's haze ice photochemistry involving polar nitriles to be significant and very similar to their non-polar counterparts.

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Particle size and abundance of HC3N ice in Titan’s lower stratosphere at high northern latitudes

Cited by 48 publications

References 30 publications

The structure of Titan’s atmosphere from Cassini radio occultations: Occultations from the Prime and Equinox missions

The structure of Titan’s atmosphere from Cassini radio occultations: Occultations from the Prime and Equinox missions

Titan’s aerosol and stratospheric ice opacities between 18 and 500μm: Vertical and spectral characteristics from Cassini CIRS

Simulation of Titan’s atmospheric photochemistry

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