Rain, winds and haze during the Huygens probe's descent to Titan's surface

M.G. Tomasko; B. Archinal; T. Becker; B. Bezard; M. Bushroe; M. Combes; D. Cook; A. Coustenis; C. De Bergh; L.E. Dafoe; L. Doose; S. Doute; A. Eibl; S. Engel; F. Gliem; B. Grieger; K. Holso; E. Howington-Kraus; E. Karkoschka; H.U. Keller; Randolph L. Kirk; R. Kramm; M. Kuppers; P. Lanagan; E. Lellouch; M. Lemmon; J. Lunine; E. McFarlane; J. Moores; G.M. Prout; B. Rizk; M. Rosiek; P. Rueffer; S.E. Schroder; B. Schmitt; C. See; P. Smith; Laurence A. Soderblom; N. Thomas; R. West

doi:10.1038/nature04126

Rain, winds and haze during the Huygens probe's descent to Titan's surface

Nature

By: M.G. Tomasko, B. Archinal, T. Becker, B. Bezard, M. Bushroe, M. Combes, D. Cook, A. Coustenis, C. De Bergh, L.E. Dafoe, L. Doose, S. Doute, A. Eibl, S. Engel, F. Gliem, B. Grieger, K. Holso, E. Howington-Kraus, E. Karkoschka, H.U. Keller, Randolph L. Kirk, R. Kramm, M. Kuppers, P. Lanagan, E. Lellouch, M. Lemmon, J. Lunine, E. McFarlane, J. Moores, G.M. Prout, B. Rizk, M. Rosiek, P. Rueffer, S.E. Schroder, B. Schmitt, C. See, P. Smith, Laurence A. Soderblom, N. Thomas, and R. West

https://doi.org/10.1038/nature04126

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Abstract

The irreversible conversion of methane into higher hydrocarbons in Titan's stratosphere implies a surface or subsurface methane reservoir. Recent measurements from the cameras aboard the Cassini orbiter fail to see a global reservoir, but the methane and smog in Titan's atmosphere impedes the search for hydrocarbons on the surface. Here we report spectra and high-resolution images obtained by the Huygens Probe Descent Imager/Spectral Radiometer instrument in Titan's atmosphere. Although these images do not show liquid hydrocarbon pools on the surface, they do reveal the traces of once flowing liquid. Surprisingly like Earth, the brighter highland regions show complex systems draining into flat, dark lowlands. Images taken after landing are of a dry riverbed. The infrared reflectance spectrum measured for the surface is unlike any other in the Solar System; there is a red slope in the optical range that is consistent with an organic material such as tholins, and absorption from water ice is seen. However, a blue slope in the near-infrared suggests another, unknown constituent. The number density of haze particles increases by a factor of just a few from an altitude of 150 km to the surface, with no clear space below the tropopause. The methane relative humidity near the surface is 50 per cent.

Additional publication details
Publication type	Article
Publication Subtype	Journal Article
Title	Rain, winds and haze during the Huygens probe's descent to Titan's surface
Series title	Nature
DOI	10.1038/nature04126
Volume	438
Issue	7069
Year Published	2005
Language	English
Publisher	Nature Research
Contributing office(s)	Astrogeology Science Center
Description	14 p.
Larger Work Type	Article
Larger Work Subtype	Journal Article
Larger Work Title	Nature
First page	765
Last page	778
Other Geospatial	Titan
Google Analytic Metrics	Metrics page