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• W1609932656 abstract "Earliest Cassini VIMS limb observations at Titan taken in October 26th, 2004 show a strong methane non-LTE limb emission at high atmospheric altitudes. During that pass at Titan, VIMS vertical resolution was about 110 km and the analyzed spectral interval corresponds to the methane emission band centered around 3.33 micron. A detailed analysis of the radiances versus altitudes shows an anomalous emission above around 900 km at wavelengths close to the methane R branch around 3.28 micron. The nature of such emission is under investigation. Different spectral databases and codes have been used for calculating the expected CH4 non-LTE limb emissions. The “anomalous” emission could not be reproduced using all the known CH4 bands. Its spectral position hints at a molecule containing C-H or C-N bonds. Different molecules and ions have been tested unsuccessfully. We propose that, given its spectral features and modeled abundances in the upper atmosphere, benzene (C6H6), the phenyl radical (C6H5) or aromatic species are likely candidate for such emission. We choose the observation on Oct. 26th, 2004 for its very good signal to noise ratio and because of the favorable illumination (low phase angle) of the atmosphere as seen from the Cassini spacecraft. Other observations also exhibit the same feature. CONCLUSIONS There are differences between the measured and expected relative behavior of the integrated intensities in the 3 branches of the methane emission. The biggest difference is due to the intensity of the R branch at high altitudes. If this difference was due to rotational NLTE effects, the relative intensity of the 3 branches should not be affected. The possibility that one particular vibration of methane could be affected by anomalous NLTE effects has been explored, but no measured hot bands could explain the observed behavior. REFERENCES Friderichsen et al., J. Am. Chem. Soc., 2001 Vuitton et al, JGR, 113, 2008 Coustenis et al., Icarus, 189, 2007 Funke et al., International Radiation Symposium, Korea, 2004 Stiller et al., JQSRT,72, 249, 2000 Yelle, ESA Spec. Publ. 1177, 243–256. Wavelength (μm) C4H6
(1,3‐butadiene) Integrated intensities & R-branch anomalies over 500 km Left panel: Spectrally integrated intensity profiles for the selected path and a 70° solar zenith angle. The anomalous behavior of the CH4 R-branch integrated intensity (cyan) has been evaluated by subtracting to the observed R-branch the calculated R-branch contribution, estimated by P-branch/1.3. Right panel: R-branches-anomaly profiles for different illumination angles Experimental Infrared Absorption Frequencies (ν), Polarizations, and Absolute Intensities for C6H5 (© JCR, 2001) Candidate molecules C6H5
(Phenyl
radical) C6H6,
C6H5
 In the upper figure modeled neutral vertical profiles and comparison with observations of C6H6 and aromatic species, are reported. The observed C6H6 mole fraction in the stratosphere was retrieved by CIRS at 15 °S [Coustenis et al., 2007]. Data points represent averages over 12 Titan passes of the C6Hx density measured by INMS. Error bars include statistic uncertainties but not calibration uncertainties (© Icarus, 2008) C6H5" @default.
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• W1609932656 date "2008-12-01" @default.
• W1609932656 modified "2023-09-23" @default.
• W1609932656 title "Anomalous emission in the 3.28 μm in the Titan upper atmosphere" @default.
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