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Near-IR Spectroscopy of the Atmosphere of Jupiter

Published online by Cambridge University Press:  14 August 2015

R.W. Carlson ,
K.H. Baines ,
T. Encrenaz ,
P. Drossart ,
M. Roos-Serote ,
F.W. Taylor ,
P. Irwin ,
A. Weir ,
P. Smith  and
S. Calcutt
R.W. Carlson
Affiliation:
Jet Propulsion Laboratory California Institute of TechnologyPasadena, CA 91109USA
K.H. Baines
Affiliation:
Jet Propulsion Laboratory California Institute of TechnologyPasadena, CA 91109USA
T. Encrenaz
Affiliation:
Observatoire de Paris-Meudon Departement SpatialeF-92195 Meudon, France
P. Drossart
Affiliation:
Observatoire de Paris-Meudon Departement SpatialeF-92195 Meudon, France
M. Roos-Serote
Affiliation:
Observatoire de Paris-Meudon Departement SpatialeF-92195 Meudon, France
F.W. Taylor
Affiliation:
Oxford University Clarendon LaboratoryOxford, OX1 3PU, UK
P. Irwin
Affiliation:
Oxford University Clarendon LaboratoryOxford, OX1 3PU, UK
A. Weir
Affiliation:
Oxford University Clarendon LaboratoryOxford, OX1 3PU, UK
P. Smith
Affiliation:
Oxford University Clarendon LaboratoryOxford, OX1 3PU, UK
S. Calcutt
Affiliation:
Oxford University Clarendon LaboratoryOxford, OX1 3PU, UK

Abstract

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The Galileo Near Infrared Mapping Spectrometer (NIMS) obtains spectral images in the wavelength range 0.7 to 5.2 μm with a spectral resolving power of approximately 200. This spectral range allows NIMS to sense cloud-reflected solar radiation, thermal emission produced in the deep atmosphere, and auroral emission from the thermosphere of Jupiter. Using 5 μm thermal emission spectroscopy, the amount of water vapor in the deep atmosphere, at approximately the (i to 8 bar level, is found to vary by a factor > 100. Deep atmosphere ammonia was also found to vary, with a spatial behavior different from that of water vapor. No evidence is found for a massive water cloud. Using reflected solar radiation in conjunction with thermal emission, two cloud layers are found, the upper at 0.5 bars and a lower one at 1-1.3 bars. The inferred absorption properties of these clouds are consistent with ammonia crystals (the upper cloud) and ammonium hydrosulfide particles (the lower cloud).

Type
III. Special Scientific Sessions
Information
Highlights of Astronomy , Volume 11 , Issue 2: Highlights of Astronomy. As presented at the XXIIIrd General Assembly of the IAU (Part B), 1997 , 1998 , pp. 1050 - 1053
Copyright
Copyright © Kluwer 1998

References

Carlson, R.W. et al. (1992) Space Sci. Rev. 60, pp. 456–502.CrossRefGoogle Scholar
Carlson, R. et al. (1996) Science, 274, pp. 385–388.CrossRefGoogle Scholar
Irwin, P.G.J., et al. (1996) J. Geophys. Res., 101, 26, pp. 137–26,154.Google Scholar
Irwin, P.G.J., et al. (1997) J. Geophys. Res., submitted.Google Scholar
Niemann, H.B. et al. (1996) Science, 272, pp. 846–848.Google Scholar
Roos-Serote, M. et al. (1997) J. Geophys. Res., submitted.Google Scholar