Exoplanet atmospheres

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WATER LOSS FROM TERRESTRIAL PLANETS WITH CO2-RICH ATMOSPHERES

The Astrophysical Journal American Astronomical Society 778:2 (2013) 154

Authors:

RD Wordsworth, RT Pierrehumbert
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Characterising Exoplanet Atmospheres with High-resolution Spectroscopy

The Messenger 154 (2013) 57-61

Authors:

J Birkby, R de Kok, M Brogi, H Schwarz, S Albrecht, E de Mooij, I Snellen

Colors of Jupiter's large anticyclones and the interaction of a Tropical Red Oval with the Great Red Spot in 2008

Journal of Geophysical Research Planets American Geophysical Union (AGU) 118:12 (2013) 2537-2557

Authors:

A Sánchez‐Lavega, J Legarreta, E García‐Melendo, R Hueso, S Pérez‐Hoyos, JM Gómez‐Forrellad, LN Fletcher, GS Orton, A Simon‐Miller, N Chanover, P Irwin, P Tanga, M Cecconi
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Searching for transits in the Wide Field Camera Transit Survey with difference-imaging light curves

Astronomy & Astrophysics EDP Sciences 560 (2013) a92

Authors:

J Zendejas Dominguez, J Koppenhoefer, RP Saglia, JL Birkby, ST Hodgkin, G Kovács, DJ Pinfield, B Sipőcz, D Barrado, R Bender, C del Burgo, M Cappetta, EL Martín, SV Nefs, A Riffeser, P Steele
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Detection of propene in titan's stratosphere

Astrophysical Journal Letters 776:1 (2013)

Authors:

CA Nixon, DE Jennings, B Bézard, S Vinatier, NA Teanby, K Sung, TM Ansty, PGJ Irwin, N Gorius, V Cottini, A Coustenis, FM Flasar

Abstract:

The Voyager 1 flyby of Titan in 1980 gave a first glimpse of the chemical complexity of Titan's atmosphere, detecting many new molecules with the infrared interferometer spectrometer (IRIS). These included propane(C3H 8) and propyne (CH3C2H), while the intermediate-sized C3Hx hydrocarbon (C3H 6) was curiously absent. Using spectra from the Composite Infrared Spectrometer on Cassini, we show the first positive detection of propene (C 3H6) in Titan's stratosphere (5σ significance), finally filling the three-decade gap in the chemical sequence. We retrieve a vertical abundance profile from 100-250 km, that varies slowly with altitude from 2.0 ± 0.8 ppbv at 125 km, to 4.6 ± 1.5 ppbv at 200 km. The abundance of C3H6 is less than both C3H 8 and CH3C2H, and we remark on an emerging paradigm in Titan's hydrocarbon abundances whereby alkanes > alkynes > alkenes within the C2Hx and C3Hx chemical families in the lower stratosphere. More generally, there appears to be much greater ubiquity and relative abundance of triple-bonded species than double-bonded, likely due to the greater resistance of triple bonds to photolysis and chemical attack. © 2013. The American Astronomical Society. All rights reserved.
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