Planetary atmosphere observation analysis

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Saturn's tropospheric composition and clouds from Cassini/VIMS 4.6-5.1 μm nightside spectroscopy

Icarus (2011)

Authors:

LN Fletcher, KH Baines, TW Momary, AP Showman, PGJ Irwin, GS Orton, M Roos-Serote, C Merlet
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Spatial and temporal variations in Titan's surface temperatures from Cassini CIRS observations

Planetary and Space Science (2011)

Authors:

V Cottini, CA Nixon, DE Jennings, R de Kok, NA Teanby, PGJ Irwin, FM Flasar
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Thermal Structure and Dynamics of Saturn's Northern Springtime Disturbance

Science (2011) 1-5

Authors:

LN Fletcher, BE Hesman, PGJ Irwin, KH Baines, TW Momary, A Sanchez-Lavega, F Michael Flasar, PL Read, GS Orton, A Simon-Miller, R Hueso, GL Bjoraker, A Mamoutkine, T Del Rio-Gaztelurrutia, JM Gomez, B Buratti, RN Clark, PD Nicholson, C Sotin

Venus's Southern Polar Vortex Reveals Precessing Circulation

Science (2011) 1-3

Authors:

D Luz, DL Berry, G Piccioni, P Drossart, R Politi, CF Wilson, S Erard, F Nuccilli

Upper limits for undetected trace species in the stratosphere of Titan

Faraday Discussions 147 (2010) 65-81

Authors:

CA Nixon, RK Achterberg, NA Teanby, PGJ Irwin, JM Flaud, I Kleiner, A Dehayem-Kamadjeu, LR Brown, RL Sams, B Bézard, A Coustenis, TM Ansty, A Mamoutkine, S Vinatier, GL Bjoraker, DE Jennings, PN Romani, FM Flasar

Abstract:

In this paper we describe the first quantitative search for several molecules in Titan's stratosphere in Cassini CIRS infrared spectra. These are: ammonia (NH3), methanol (CH3OH), formaldehyde (H 2CO), and acetonitrile (CH3CN), all of which are predicted by photochemical models but only the last of which has been observed, and not in the infrared. We find non-detections in all cases, but derive upper limits on the abundances from low-noise observations at 25°S and 75°N. Comparing these constraints to model predictions, we conclude that CIRS is highly unlikely to see NH3 or CH3OH emissions. However, CH3CN and H2CO are closer to CIRS detectability, and we suggest ways in which the sensitivity threshold may be lowered towards this goal. © 2010 The Royal Society of Chemistry.
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