New infrared integrated band intensities for HC3N and extensive line list for the ν5 and ν6 bending modes

Jolly, A.; Bénilan, Y.; Fayt, André

doi:10.1016/j.jms.2007.01.008

Cited by 37 publications

(43 citation statements)

References 22 publications

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“…The next band to be observed in HC 5 N is the 2m 7 overtone at 1272 cm À1 . It has an intensity ratio compared to the fundamental m 7 CCH bending mode which is about one third, approximately the same as the one observed between the equivalent m 5 fundamental CCH bending mode and its 2m 5 overtone for HC 3 N [19]. In addition to the strong m 7 bending mode at 642 cm À1 , we also observe two more bending modes, m 8 at 501 cm À1 and m 9 at 461 cm À1 (Fig.…”

Section: Bands Position and Relative Intensitiessupporting

confidence: 79%

Infrared band intensities of cyanobutadiyne (HC5N) between 400 and 4000cm−1

Bénilan¹,

Jolly²,

Trolez³

et al. 2007

Journal of Molecular Spectroscopy

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Section: Bands Position and Relative Intensitiessupporting

confidence: 79%

Infrared band intensities of cyanobutadiyne (HC5N) between 400 and 4000cm−1

Bénilan¹,

Jolly²,

Trolez³

et al. 2007

Journal of Molecular Spectroscopy

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“…The Lorentz halfwidths were set to 0:1 cm À1 atm À1 for all lines, varying as T À0:75 . For HC 3 N, we used the linelist from Jolly et al (2007) with Lorentz half-widths of 0:1 cm À1 atm À1 varying as T À0:75 .…”

Section: Retrieval Methods and Radiative Transfer Modelmentioning

confidence: 99%

Analysis of Cassini/CIRS limb spectra of Titan acquired during the nominal mission

Vinatier

Bézard

Nixon

et al. 2010

Icarus

180

182

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“…The altitude scale of the atmospheric profiles were determined by assuming hydrostatic equilibrium and an altitude/latitude‐dependent gravity: this required us to make reasonable assumptions about temperatures in the lower stratosphere and troposphere, which were unconstrained by these observations. Spectroscopic parameters were the same as from Teanby et al [2007] except that we have used updated line data for HC 3 N from Jolly et al [2007].…”

Section: Methodsmentioning

confidence: 99%

Titan's winter polar vortex structure revealed by chemical tracers

et al. 2008

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[1] The winter polar vortex on Saturn's largest moon Titan has profound effects on atmospheric circulation and chemistry and for the current northern midwinter season is the major dynamical feature of Titan's stratosphere and mesosphere. We use 2 years of observations from Cassini's composite infrared spectrometer to determine cross sections of five independent chemical tracers (HCN, HC 3 N, C 2 H 2 , C 3 H 4 , and C 4 H 2 ), which are then used to probe dynamical processes occurring within the vortex. Our results provide compelling evidence that the vortex acts as a strong mixing barrier in the stratosphere and mesosphere, effectively separating a tracer-enriched air mass in the north from air at lower latitudes. In the mesosphere, above the level of the vortex jet, a tracer-depleted zone extends away from the north pole toward the equator and enrichment is confined to high northern latitudes. However, below this level, mixing processes cause tongues of gas to extend away from the polar region toward the equator. These features are not reproduced by current general circulation models and suggest that a residual polar circulation is present and that waves and instabilities form a more important part of Titan's atmospheric dynamics than previously thought. We also observe an unexpected enrichment of C 4 H 2 in the northern stratosphere, which suggests photochemical polymerization of C 2 H 2 . Our observations provide stringent new constraints for dynamical and photochemical models and identify key polar processes for the first time. Some of the processes we see have analogues in Earth's polar vortex, while others are unique to Titan.

show abstract

New infrared integrated band intensities for HC3N and extensive line list for the ν5 and ν6 bending modes

Cited by 37 publications

References 22 publications

Infrared band intensities of cyanobutadiyne (HC5N) between 400 and 4000cm−1

Infrared band intensities of cyanobutadiyne (HC5N) between 400 and 4000cm−1

Analysis of Cassini/CIRS limb spectra of Titan acquired during the nominal mission

Titan's winter polar vortex structure revealed by chemical tracers

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