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Published Online May 30, 2002
Science DOI: 10.1126/science.1073541

Reports

Submitted on May 2, 2002
Accepted on May 21, 2002

Global Distribution of Neutrons from Mars: Results from Mars Odyssey

W. C. Feldman 1*, W. V. Boynton 2, R. L. Tokar 1, T. H. Prettyman 1, O. Gasnault 1, S. W. Squyres 3, R. C. Elphic 1, D. J. Lawrence 1, S. L. Lawson 1, S. Maurice 4, G. W. McKinney 1, K. R. Moore 1, R. C. Reedy 1

1 Los Alamos National Laboratory, Los Alamos, NM 87545, USA.
2 University of Arizona, Lunar Planetary Laboratory, Tucson, AZ 85721, USA.
3 Cornell University, Center for Radiophysics and Space Research, Ithaca, NY 14853, USA.
4 Observatoire Midi-Pyrénées, 31400 Toulouse, France.

* To whom correspondence should be addressed. E-mail: wfeldman{at}lanl.gov.

Global distributions of thermal, epithermal, and fast neutron fluxes have been mapped during late southern summer/northern winter using the Mars Odyssey Neutron Spectrometer. These fluxes are selectively sensitive to the vertical and lateral spatial distributions of H and CO2 in the uppermost meter of the Martian surface. Poleward of ±60° latitude is terrain rich in hydrogen, probably H2O ice buried beneath tens of centimeter-thick hydrogen-poor soil. The central portion of the north polar cap is covered by a thick CO2 layer, as is the residual south polar cap. Portions of the low to middle latitudes indicate subsurface deposits of chemically and/or physically bound H2O and/or OH.


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