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Distribución global de neutrones de Marte: resultados de la odisea de Marte
W C Feldman1, W V Boynton, R L Tokar
1Los Alamos National Laboratory, Los Alamos, NM 87545, USA. wfeldman@lanl.gov
Science (New York, N.Y.)
|June 1, 2002
Resumen
El mapeo global del flujo de neutrones revela hielo de agua marciano y depósitos de dióxido de carbono. Las regiones ricas en hidrógeno hacia los polos de 60 grados de latitud probablemente contengan hielo de agua enterrado, mientras que las capas polares muestran un significativo dióxido de carbono. Los depósitos de agua subterránea también están indicados en latitudes más bajas.
Área de la Ciencia:
- Ciencias planetarias Ciencias planetarias.
- Astrogeología y Astrogeología.
- La geofísica es la geofísica.
Sus antecedentes:
- Comprender la distribución del hidrógeno y el dióxido de carbono es crucial para caracterizar el clima pasado y presente de Marte.
- El espectrómetro de neutrones Mars Odyssey (MONS) proporciona un conjunto de datos único para mapear estos elementos volátiles en el subsuelo marciano.
Objetivo del estudio:
- Mapear la distribución global de los flujos de neutrones térmicos, epitermales y rápidos en Marte.
- Para inferir la distribución espacial del hidrógeno (como H2O) y el dióxido de carbono (CO2) en el entorno cercano a la superficie.
Principales métodos:
- Se utilizaron datos del espectrómetro de neutrones Mars Odyssey (MONS).
- Mediciones de flujo de neutrones analizadas sensibles al contenido de hidrógeno y CO2.
- Distribuciones mapeadas durante el verano tardío del sur / invierno del norte.
Principales resultados:
- Terreno rico en hidrógeno identificado hacia el polo de +/-60 grados de latitud, indicativo de hielo de agua enterrado.
- Se observó una gruesa capa de dióxido de carbono que cubre la capa polar norte central y la capa polar sur residual.
- Se ha detectado evidencia de depósitos subterráneos de agua unida (H2O) y/o hidroxilo (OH) en latitudes bajas y medias.
Conclusiones:
- El estudio proporciona un mapa global de las principales distribuciones volátiles en Marte.
- Los hallazgos sugieren importantes reservas de hielo de agua en latitudes altas y hielo de CO2 en los polos.
- La evidencia de agua unida / OH en latitudes más bajas garantiza una mayor investigación de los procesos de hidratación marciana.
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