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Originally published in Science Express on 19 August 2004
Science 10 September 2004:
Vol. 305. no. 5690, pp. 1582 - 1586
DOI: 10.1126/science.1100240
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Research Articles

Jupiter's Atmospheric Composition from the Cassini Thermal Infrared Spectroscopy Experiment

V. G. Kunde,1* F. M. Flasar,2 D. E. Jennings,2 B. Bézard,3 D. F. Strobel,4 B. J. Conrath,5 C. A. Nixon,1 G. L. Bjoraker,2 P. N. Romani,2 R. K. Achterberg,6 A. A. Simon-Miller,2 P. Irwin,7 J. C. Brasunas,2 J. C. Pearl,2 M. D. Smith,2 G. S. Orton,8 P. J. Gierasch,5 L. J. Spilker,8 R. C. Carlson,6 A. A. Mamoutkine,6 S. B. Calcutt,7 P. L. Read,7 F. W. Taylor,7 T. Fouchet,3 P. Parrish,7 A. Barucci,3 R. Courtin,3 A. Coustenis,3 D. Gautier,3 E. Lellouch,3 A. Marten,3 R. Prangé,3 Y. Biraud,3 C. Ferrari,9 T. C. Owen,10 M. M. Abbas,11 R. E. Samuelson,1 F. Raulin,12 P. Ade,13 C. J. Césarsky,14 K. U. Grossman,15 A. Coradini16

The Composite Infrared Spectrometer observed Jupiter in the thermal infrared during the swing-by of the Cassini spacecraft. Results include the detection of two new stratospheric species, the methyl radical and diacetylene, gaseous species present in the north and south auroral infrared hot spots; determination of the variations with latitude of acetylene and ethane, the latter a tracer of atmospheric motion; observations of unexpected spatial distributions of carbon dioxide and hydrogen cyanide, both considered to be products of comet Shoemaker-Levy 9 impacts; characterization of the morphology of the auroral infrared hot spot acetylene emission; and a new evaluation of the energetics of the northern auroral infrared hot spot.

1 Department of Astronomy, University of Maryland, College Park, MD 20742, USA.
2 NASA/Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA.
3 LESIA, CNRS-UMR8109, Observatoire de Paris, 5 place Jules Janssen, F-91925 Meudon Cedex, France.
4 Johns Hopkins University, Department of Earth and Planetary Science, Baltimore, MD 21218, USA.
5 Department of Astronomy, Cornell University, Ithaca, NY 14853, USA.
6 Space Science and Applications, Inc., 5900 Princess Garden Parkway, Suite 300, Lanham, MD 20706, USA.
7 Atmospheric, Oceanic, and Planetary Physics, Clarendon Laboratory, Parks Road, University of Oxford, Oxford OX1 3PU, UK.
8 Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA.
9 CEA Saclay, Service d'Astrophysique, 91191 Gif-sur-Yvette Cedex, France.
10 University of Hawaii, Institute of Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA.
11 NASA/Marshall Space Flight Center, SD50, Huntsville, AL 35812, USA.
12 LISA, Université de Paris 7 and 12, CNRS–UMR 7583, 61 Avenue General de Gaulle, 94010 Creteil Cedex, France.
13 School of Physics and Astronomy, Cardiff University, 5 The Parade, Cardiff CF24 3YB, UK.
14 European Southern Observatory, Karl-Schwarzschild-strasse 2, 85748 Garching bei Muenchen, Germany.
15 Gesamthochschule Wuppertal, Department of Physics, Gausstrasse 20, 5600 Wuppertal 1, Germany.
16 Instituto di Astrofisica Spaziale–CNR, Area della recerca di Tor Vergata, via del Fosso del Cavaliere 100, Rome, I-00133 Italy.

* To whom correspondence should be addressed. E-Mail: Virgil.G.Kunde.1{at}gsfc.nasa.gov

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THIS ARTICLE HAS BEEN CITED BY OTHER ARTICLES:
Oxygen and Other Volatiles in the Giant Planets and their Satellites.
M. H. Wong, J. I. Lunine, S. K. Atreya, T. Johnson, P. R. Mahaffy, T. C. Owen, and T. Encrenaz (2008)
Reviews in Mineralogy and Geochemistry 68, 219-246
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