IR and UV spectroscopic studies at low temperature: C2N2

Details IR and UV spectroscopic studies at low temperature: C2N2 IR and UV spectroscopic studies at low temperature: C2N2

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008epsc.conf..916b&link_type=abstract

European Planetary Science Congress 2008, Proceedings of the conference held 21-25 September, 2008 in Münster, Germany. Online a

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Titan's atmosphere is mainly made of nitrogen and methane and is furthermore very rich in organic molecules. Hydrocarbons are formed by the photodissociation of CH4 and nitriles are created by dissociation of N2 followed by reactions with hydrocarbons. In order to understand the physicochemical mechanisms responsible for the evolution of Titan's atmosphere, photochemical models are built. The latter needs constraints for the determination of vertical profiles of organic compounds, from the higher thermosphere down to the lower stratosphere. They also need wavelength dependant photodissociation rates as input parameters. Vertical profiles can be retrieved from Cassini observations along the entire atmosphere, in particular by limb sounding using Cassini's UVIS and CIRS spectrometers. However, in order to interpret data obtained by these instruments, precise spectroscopic parameters and their dependence on temperature are needed. We will review the current knowledge in this field of planetary spectroscopy and point out the lack of spectroscopic parameters of already detected species. These parameters are especially needed for radiative transfer calculations at low temperatures. We will focus our talk on the Cyanogen molecule (C2N2) which has been observed in Titan's atmosphere in the FIR domain, around 230 cm-1. We will present the latest spectroscopic studies we have performed on this molecule which cover the entire spectrum from the mid- infrared to the vacuum ultraviolet spectral region. Integrated band intensities have been determined for all bands in the infrared. In the ultraviolet domain, we have determined absolute cross sections from 350 down to 80 nm covering six orders of magnitude for the absorption coefficient. We will also show how temperature can influence VUV absorption coefficients. The corresponding implications of temperature dependant absorption data on the interpretation of UVIS observations will be discussed.

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