DOI: 10.1126/science.1081897. Evidence for the Exposure of Water Ice on Titan's Surface

Evidence for the Exposure of Water Ice on Titan's Surface

10.1126/science.1081897

Crossref journal-article

American Association for the Advancement of Science (AAAS)

Science (221)

Abstract

The smoggy stratosphere of Saturn's largest moon, Titan, veils its surface from view, except at narrow wavelengths centered at 0.83, 0.94, 1.07, 1.28, 1.58, 2.0, 2.9, and 5.0 micrometers. We derived a spectrum of Titan's surface within these “windows” and detected features characteristic of water ice. Therefore, despite the hundreds of meters of organic liquids and solids hypothesized to exist on Titan's surface, its icy bedrock lies extensively exposed.

Bibliography

Griffith, C. A., Owen, T., Geballe, T. R., Rayner, J., & Rannou, P. (2003). Evidence for the Exposure of Water Ice on Titanâs Surface. Science, 300(5619), 628â630.

Authors 5

Caitlin A. Griffith (first)
Tobias Owen (additional)
Thomas R. Geballe (additional)
John Rayner (additional)
Pascal Rannou (additional)

References 53 Referenced 134

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10.1126/science.221.4605.55
10.1126/science.222.4629.1229
10.1016/0019-1035(91)90219-J
10.1006/icar.1995.1179
Haze optical constants come from Khare et al. ( 39 ).
Spectra of decade-old tholins ( 40 ) differ at 1.2 to 1.4 μm from spectra of young tholins ( 41 ). It is not clear whether the tholin chemistry proceeded in isolation or through contamination.
Noll et al. ( 42 ) do not consider scattering and emission causing slightly different results from ours at 5 μm.
10.1038/26920
J. T. Rayner et al., Publ. Astron. Soc. Pac.115, 362 (2003). (10.1086/367745) / Publ. Astron. Soc. Pac. (2003)
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O. B. Toon, C. P. McKay, C. A. Griffith, R. P. Turco, Icarus95, 24 (1992). (10.1016/0019-1035(92)90188-D) / Icarus (1992)
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We adopted a discrete ordinates calculation having eight streams as described by Stamnes et al. ( 43 ).
Titan's thermal profile derives from Lellouch et al. ( 44 ) and Yelle et al. ( 45 ).
Absorption coefficients of CH 4 and CO derive from the line parameters of Husson et al. ( 46 ).
We varied the vertical optical depth at two altitude regions (40 to 100 km and 100 to 160 km) to derive the range of haze optical depths that fit Titan's spectrum. Haze below ∼40 km is limited by the visibility of Titan's surface at 0.63 μm.
Our surface albedos are thus unaffected by variations in the 0.01 shape parameter (or width) of our log-normal particle distribution the tholin optical constants ( 6 ) and details of the haze models.
K. Rages, J. B. Pollack, P. H. Smith, J. Geophys. Res.88, 8721 (1983). (10.1029/JA088iA11p08721) / J. Geophys. Res. (1983)
10.1006/icar.1996.0023
J. Richardson R. D. Lorenz A. McEwen in preparation.
M. G. Tomasko, P. H. Smith, Icarus51, 65 (1982). (10.1016/0019-1035(82)90030-6) / Icarus (1982)
R. A. West et al., J. Geophys. Res.88, 8699 (1983). (10.1029/JA088iA11p08699) / J. Geophys. Res. (1983)
R. A. West, P. H. Smith, Icarus90, 330 (1991). (10.1016/0019-1035(91)90113-8) / Icarus (1991)
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One model that fits our optical depths contains haze above 90-km altitude where the radius (in micrometers) column abundance (km amagat) and 0.94-μm optical depth are specified by the values ( a b c ) of (6.8 –424 0) (152.3 –131.7 –34.5) and (104.3 –108.9 –20.2) respectively. These haze parameters x depend on altitude z (in km) as: z = a + b log 10 ( x ) + c [log 10 ( x )] 2 .
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Methane is assumed to be subsaturated at the surface with a humidity of 60%. A constant mixing ratio is adopted above the surface until the level of saturation is reached. Above this level the atmosphere is saturated up to the tropopause. The mixing ratio is constant at the tropopause value above this point. An amagat is a unit of density equal to 2.69 × 10 19 cm - 3 .
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We thank D. Cruikshank for helpful discussions regarding the spectroscopic characteristics of complex organic molecules. This research is supported by the NASA Planetary Astronomy Program.

Dates

Type	When
Created	22 years, 4 months ago (April 25, 2003, 8:15 a.m.)
Deposited	1 year, 7 months ago (Jan. 9, 2024, 11:40 p.m.)
Indexed	3 weeks ago (Aug. 5, 2025, 9:07 a.m.)
Issued	22 years, 4 months ago (April 25, 2003)
Published	22 years, 4 months ago (April 25, 2003)
Published Print	22 years, 4 months ago (April 25, 2003)

Funders 0

None

BibTeX

@article{Griffith_2003, title={Evidence for the Exposure of Water Ice on Titan’s Surface}, volume={300}, ISSN={1095-9203}, url={http://dx.doi.org/10.1126/science.1081897}, DOI={10.1126/science.1081897}, number={5619}, journal={Science}, publisher={American Association for the Advancement of Science (AAAS)}, author={Griffith, Caitlin A. and Owen, Tobias and Geballe, Thomas R. and Rayner, John and Rannou, Pascal}, year={2003}, month=apr, pages={628–630} }

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