La formación de recientes flujos de escombros marcianos por el derretimiento del hielo subterráneo cercano a la superficie a alta oblicuidad
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Simulation of the Planetary Interior Differentiation Processes in the Laboratory
Published on: November 15, 2013
F Costard1, F Forget, N Mangold
1UMR8616, Centre National de la Recherche Scientifique (CNRS), OrsayTerre, Equipe de Géomorphologie Planétaire, Université Paris-Sud, 91405, Orsay Cedex, France.
Science (New York, N.Y.)
|December 1, 2001
Resumen
La escorrentía superficial reciente en Marte sugiere agua líquida. Una nueva investigación indica que los barrancos marcianos pueden formarse por el derretimiento del hielo subterráneo en alta oblicuidad, no por filtración de agua subterránea.
Área de la Ciencia:
- Ciencias planetarias Ciencias planetarias.
- Geología Geología Geología.
- Hidrología Hidrología Hidrología.
Sus antecedentes:
- Observaciones recientes de pequeños barrancos y escurrimientos superficiales en Marte han reavivado las discusiones sobre la estabilidad del agua líquida en la superficie marciana.
- Las teorías existentes sugieren que la filtración de agua subterránea de los acuíferos es la causa, pero los barrancos que se forman en picos aislados y crestas de dunas desafían esta hipótesis.
Objetivo del estudio:
- Para investigar una hipótesis alternativa para la formación de barrancos marcianos.
- Para determinar si el derretimiento del hielo de agua subterránea en alta oblicuidad podría explicar las características de barrancos observadas.
Principales métodos:
- Análisis comparativo de barrancos marcianos con flujos de escombros terrestres en Groenlandia.
- Simulaciones numéricas para modelar las condiciones de temperatura cercanas a la superficie en Marte a alta oblicuidad.
Principales resultados:
- El estudio encontró que las temperaturas por encima del punto de congelación pueden ocurrir en la superficie cercana de Marte en alta oblicuidad.
- Estas temperaturas pronosticadas se correlacionan con las latitudes y orientaciones de pendiente específicas donde se observan los barrancos marcianos.
- Los hallazgos apoyan el derretimiento del hielo de agua subterránea como un mecanismo plausible de formación de barrancos.
Conclusiones:
- Es probable que los barrancos marcianos se formen por el derretimiento del hielo de agua subterránea poco profunda durante los períodos de alta oblicuidad.
- Este proceso ofrece una explicación más consistente para los barrancos observados en diversos terrenos marcianos que la filtración de agua subterránea.
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