The identification of liquid ethane in Titan’s Ontario Lacus.

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Title: The identification of liquid ethane in Titan’s Ontario Lacus.
Authors: Brown, R. H., Soderblom, L. A., Soderblom, J. M., Clark, R. N., Jaumann, R., Barnes, J. W., Sotin, C., Buratti, B., Baines, K. H., Nicholson, P. D.
Source: Nature. 7/31/2008, Vol. 454 Issue 7204, p607-610. 4p. 1 Color Photograph, 4 Graphs.
Subjects: Titan (Satellite) research, Space exploration, Satellites of Saturn, Ethanes, Liquefied gases, Lake hydrology, Cartography, Methane, Hydrocarbons
Abstract: Titan was once thought to have global oceans of light hydrocarbons on its surface, but after 40 close flybys of Titan by the Cassini spacecraft, it has become clear that no such oceans exist. There are, however, features similar to terrestrial lakes and seas, and widespread evidence for fluvial erosion, presumably driven by precipitation of liquid methane from Titan’s dense, nitrogen-dominated atmosphere. Here we report infrared spectroscopic data, obtained by the Visual and Infrared Mapping Spectrometer (VIMS) on board the Cassini spacecraft, that strongly indicate that ethane, probably in liquid solution with methane, nitrogen and other low-molecular-mass hydrocarbons, is contained within Titan’s Ontario Lacus. [ABSTRACT FROM AUTHOR]
Copyright of Nature is the property of Springer Nature and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
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  Data: The identification of liquid ethane in Titan’s Ontario Lacus.
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  Data: <searchLink fieldCode="DE" term="%22Titan+%28Satellite%29+research%22">Titan (Satellite) research</searchLink><br /><searchLink fieldCode="DE" term="%22Space+exploration%22">Space exploration</searchLink><br /><searchLink fieldCode="DE" term="%22Satellites+of+Saturn%22">Satellites of Saturn</searchLink><br /><searchLink fieldCode="DE" term="%22Ethanes%22">Ethanes</searchLink><br /><searchLink fieldCode="DE" term="%22Liquefied+gases%22">Liquefied gases</searchLink><br /><searchLink fieldCode="DE" term="%22Lake+hydrology%22">Lake hydrology</searchLink><br /><searchLink fieldCode="DE" term="%22Cartography%22">Cartography</searchLink><br /><searchLink fieldCode="DE" term="%22Methane%22">Methane</searchLink><br /><searchLink fieldCode="DE" term="%22Hydrocarbons%22">Hydrocarbons</searchLink>
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  Data: Titan was once thought to have global oceans of light hydrocarbons on its surface, but after 40 close flybys of Titan by the Cassini spacecraft, it has become clear that no such oceans exist. There are, however, features similar to terrestrial lakes and seas, and widespread evidence for fluvial erosion, presumably driven by precipitation of liquid methane from Titan’s dense, nitrogen-dominated atmosphere. Here we report infrared spectroscopic data, obtained by the Visual and Infrared Mapping Spectrometer (VIMS) on board the Cassini spacecraft, that strongly indicate that ethane, probably in liquid solution with methane, nitrogen and other low-molecular-mass hydrocarbons, is contained within Titan’s Ontario Lacus. [ABSTRACT FROM AUTHOR]
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  Data: <i>Copyright of Nature is the property of Springer Nature and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract.</i> (Copyright applies to all Abstracts.)
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