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Distribuciones de hielo de agua subterránea de alta resolución en Marte.
1School of Earth and Space Exploration, Arizona State University, Tempe, Arizona 85287-6305, USA. joshband@asu.edu
Nature
|May 4, 2007
Resumen
El hielo de agua es estable en el subsuelo poco profundo de Marte, con su profundidad variando según la latitud. Las nuevas imágenes térmicas revelan variaciones localizadas, lo que sugiere un ciclo de agua marciano activo y factores que influyen en la profundidad de la capa de hielo.
Área de la Ciencia:
- Ciencias planetarias Ciencias planetarias.
- La geofísica es la geofísica.
Sus antecedentes:
- Los modelos teóricos predicen el hielo de agua estable en el subsuelo poco profundo de Marte (<1-2 m) en latitudes altas.
- La detección previa de hidrógeno por el espectrómetro de rayos gamma (GRS) apoyó modelos de aumento de la profundidad de la tabla de hielo con la disminución de la latitud.
- Las mediciones anteriores estaban limitadas por la huella del GRS, lo que dificultaba la observación detallada de la distribución del hielo.
Objetivo del estudio:
- Para investigar las heterogeneidades a escala subkilométrica en la distribución del hielo de agua subterránea marciana.
- Para analizar la influencia de las características de la superficie local y las propiedades térmicas en la profundidad de la tabla de hielo.
- Para evaluar las implicaciones para el ciclo actual del agua de Marte y la dinámica climática.
Principales métodos:
- Utilizó el Sistema de Imágenes de Emisión Térmica (THEMIS) en Mars Odyssey para observar las respuestas estacionales de la temperatura de la superficie.
- Se analizaron datos térmicos para inferir las propiedades del subsuelo y la distribución del hielo de agua a escalas subkilométricas.
- Comparó datos de observación con modelos teóricos de la estabilidad del hielo de agua y el intercambio atmosférico.
Principales resultados:
- Demostró la capacidad de observar las heterogeneidades superficiales que influyen en la profundidad del hielo de agua a escalas sub-kilométricas.
- Reveló una significativa variabilidad regional y local en la profundidad del hielo de agua, consistente con algunos modelos atmosféricos.
- Regiones identificadas con desviaciones de la estabilidad teórica, lo que indica factores adicionales que influyen en la profundidad de la capa de hielo.
Conclusiones:
- La distribución del hielo de agua subterránea marciana es muy variable a escalas locales.
- Las observaciones apoyan un ciclo de agua marciano activo que responde a los ciclos climáticos orbitales.
- Se necesita más investigación para comprender los factores que causan desviaciones de las profundidades teóricas de estabilidad del hielo.
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