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Valles marcianos: morfología, distribución, edad y origen
Science (New York, N.Y.)
|November 21, 1980
Resumen
Las redes de valles de Marte probablemente se formaron por absorción basal, no por lluvia. La evidencia sugiere que estas antiguas características geológicas marcianas no han cambiado en miles de millones de años.
Área de la Ciencia:
- Geología planetaria Geología planetaria.
- Geomorfología Geomorfología.
- Astrobiología Astrobiología.
Sus antecedentes:
- Las redes de valles ramificados son comunes en Marte.
- Las hipótesis anteriores sugirieron la erosión alimentada por las lluvias como un mecanismo de formación primaria.
Objetivo del estudio:
- Para investigar los mecanismos de formación de las redes de valles marcianos.
- Para determinar la edad de la formación de los valles marcianos.
Principales métodos:
- Análisis de la morfología de la red de valles (difusión, ángulos tributarios, áreas de intervalo).
- Examen de las características del cañón (terminaciones, topografía de la pared, control estructural).
- Comparación de las distribuciones tamaño-frecuencia de los cráteres de impacto dentro de los valles y el terreno circundante.
Principales resultados:
- Las redes de valles muestran patrones de erosión ineficientes incompatibles con las precipitaciones.
- Las características del cañón sugieren una extensión hacia adelante impulsada por el sapping basal.
- Las distribuciones de los cráteres de impacto indican que no hubo formación de valles significativos durante miles de millones de años.
Conclusiones:
- El absorción basal es un mecanismo más plausible para la formación de la red de valles marcianos que la lluvia.
- La formación de valles en Marte cesó hace miles de millones de años, lo que indica un pasado geológico estable.
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