Distribution of Hydrogen in the Near Surface of Mars: Evidence for Subsurface Ice Deposits-Reference-Cited by-同舟云学术

Distribution of Hydrogen in the Near Surface of Mars: Evidence for Subsurface Ice Deposits

Published:2002-07-05 Issue:5578 Volume:297 Page:81-85
ISSN:0036-8075
Container-title:Science
language:en
Short-container-title:Science

Author:

Boynton W. V.¹,Feldman W. C.²,Squyres S. W.³,Prettyman T. H.²,Brückner J.⁴,Evans L. G.⁵,Reedy R. C.²⁶,Starr R.⁷,Arnold J. R.⁸,Drake D. M.⁹,Englert P. A. J.¹⁰,Metzger A. E.¹¹,Mitrofanov Igor¹²,Trombka J. I.¹³,d'Uston C.¹⁴,Wänke H.⁴,Gasnault O.¹⁴,Hamara D. K.¹,Janes D. M.¹,Marcialis R. L.¹,Maurice S.¹⁵,Mikheeva I.¹,Taylor G. J.¹⁶,Tokar R.²,Shinohara C.¹

Affiliation:

1. Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA.

2. Los Alamos National Laboratory, Los Alamos, NM 87545, USA.

3. Center for Radiophysics & Space Research, Cornell University, Ithaca, NY 14853, USA.

4. Max-Planck-Institut für Chemie, 55020 Mainz, Federal Republic of Germany.

5. Science Programs, Computer Sciences Corporation, Lanham, MD 20706, USA.

6. Institute of Meteoritics, University of New Mexico, Albuquerque, NM 87131, USA.

7. Department of Physics, The Catholic University of America, Washington, DC 20064, USA.

8. Department of Chemistry, University of California San Diego, La Jolla, CA 92093, USA.

9. TechSource, Sante Fe, NM 87505, USA.

10. Victoria University of Wellington, Wellington, New Zealand.

11. Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA.

12. Space Research Institute, Moscow, Russia.

13. NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA.

14. Centre d'Etude Spatiale des Rayonnements, Toulouse, France.

15. Observatoire Midi-Pyrenees, 31400 Toulouse, France.

16. University of Hawaii, Honolulu, HI 96822, USA.

Abstract

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° latitude to about 40 grams per square centimeter at –77°. 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.

Publisher

American Association for the Advancement of Science (AAAS)

Subject

Multidisciplinary

Reference27 articles.

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2. Water and the martian landscape

3. Martian North Pole Summer Temperatures: Dirty Water Ice

4. Evidence for Recent Groundwater Seepage and Surface Runoff on Mars

5. Evidence for recent climate change on Mars from the identification of youthful near-surface ground ice

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