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Volumn 280, Issue 5369, 1998, Pages 1576-1580

Detection of atomic deuterium in the upper atmosphere of Mars

Author keywords

[No Author keywords available]

Indexed keywords

DEUTERIUM; HYDROGEN; WATER;

EID: 0032486324     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.280.5369.1576     Document Type: Article
Times cited : (107)

References (59)
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    • 2O vapor in the lower atmosphere.
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    • 2, which are similar to those of HD in (27) and taken from the same sources. As for HD, the model reflects the global mean conditions but for solar maximum. These differ from the daytime conditions of the model in (4). Temperature, ion density, and eddy diffusion profiles are taken from the solar maximum model in (6).
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    • 2O between them is slow and reservoirs do not completely disappear. This assumption is questionable.
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    • e = 30 m. Our model differs from the model (12) in which reservoir two is disconnected from reservoir one and gradually shrinks from 3.6 to 0.2 m.
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    • V.A.K. thanks T. Reyes for consulting in data processing. This work was supported by the HST Guest Observer Program.


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