| Autor: |
Boynton WV; Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA. wboynton@lpl.arizona.edu, Feldman WC, Squyres SW, Prettyman TH, Bruckner J, Evans LG, Reedy RC, Starr R, Arnold JR, Drake DM, Englert PA, Metzger AE, Mitrofanov I, Trombka JI, D'Uston C, Wanke H, Gasnault O, Hamara DK, Janes DM, Marcialis RL, Maurice S, Mikheeva I, Taylor GJ, Tokar R, Shinohara C |
| Jazyk: |
angličtina |
| Zdroj: |
Science (New York, N.Y.) [Science] 2002 Jul 05; Vol. 297 (5578), pp. 81-5. Date of Electronic Publication: 2002 May 30. |
| DOI: |
10.1126/science.1073722 |
| Abstrakt: |
Using the Gamma-Ray Spectrometer on the Mars Odyssey, we have identified two regions near the poles that are enriched in hydrogen. The data indicate the presence of a subsurface layer enriched in hydrogen overlain by a hydrogen-poor layer. The thickness of the upper layer decreases with decreasing distance to the pole, ranging from a column density of about 150 grams per square centimeter at -42 degrees latitude to about 40 grams per square centimeter at -77 degrees. The hydrogen-rich regions correlate with regions of predicted ice stability. We suggest that the host of the hydrogen in the subsurface layer is ice, which constitutes 35 +/- 15% of the layer by weight. |
| Databáze: |
MEDLINE |
| Externí odkaz: |
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