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Formación de aguas subterráneas de los valles marcianos

M C Malin¹, M H Carr

¹Malin Space Science Systems, San Diego, California 92191-0148, USA. malin@mss.com

|March 2, 1999

Resumen

Las aguas subterráneas, no el escurrimiento superficial, probablemente dieron forma a las redes de valles de Marte. Las imágenes de alta resolución revelan que los procesos de agua subterránea fueron clave para formar estas características geológicas marcianas.

Área de la Ciencia:

Ciencias planetarias Ciencias planetarias.
Geología Geología Geología.
Hidrología Hidrología Hidrología.

Sus antecedentes:

Marte exhibe grandes canales de salida atribuidos a antiguas inundaciones.
Las redes de valles más pequeñas y ramificadas con afluentes presentan un origen controvertido.
Las hipótesis existentes incluyen la escorrentía superficial (Marte temprano / tardío) o los procesos de agua subterránea / hielo subterráneo.

Objetivo del estudio:

Para investigar los mecanismos de formación de las redes de valles marcianos.
Para determinar el papel de las aguas subterráneas en la formación de estos valles.
Para analizar imágenes de alta resolución de los valles marcianos.

Principales métodos:

Análisis de imágenes de alta resolución de los valles marcianos.
Comparación de la morfología del valle con los procesos geológicos conocidos.

Principales resultados:

Las imágenes de alta resolución apoyan un papel importante para las aguas subterráneas en la formación de valles.
La evidencia sugiere que los procesos de agua subterránea fueron activos en la conformación de los valles marcianos.
El momento preciso de estos eventos de aguas subterráneas sigue siendo indeterminado.

Conclusiones:

Las aguas subterráneas jugaron un papel crucial en la formación de las redes de valles marcianos.
La escorrentía superficial es menos probable que sea la causa principal de estos valles.
Se necesita más investigación para establecer el momento de estos eventos de agua subterránea.

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