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Tres años en Marte: el módulo de aterrizaje viking 1 toma imágenes de las observaciones.

R E Arvidson, E A Guinness, H J Moore

Science (New York, N.Y.)

|November 4, 1983

Resumen

Marte Marte es el planeta Marte.

Área de la Ciencia:

Ciencias planetarias Ciencias planetarias.
Procesos de la superficie de Marte Procesos de la superficie de Marte
Ciencias atmosféricas en Marte.

Sus antecedentes:

La Estación Conmemorativa Mutch (Viking Lander 1) recogió datos en Marte durante 2245 días marcianos.
Estudios anteriores no han detallado completamente la deposición de polvo marciano y la dinámica de la erosión.
Comprender la estabilidad de la superficie marciana es crucial para la exploración futura.

Objetivo del estudio:

Para analizar la deposición de polvo marciano y los patrones de erosión.
Investigar el papel de las tormentas de polvo en la redistribución del material superficial.
Comprender los factores que influyen en la cohesión y estabilidad del suelo marciano.

Principales métodos:

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Análisis de imágenes y datos meteorológicos del Viking Lander 1.

Correlación de los datos de presión atmosférica con los eventos de erosión observados.

Examen de los cambios en la superficie en relación con la actividad de las tormentas de polvo y las interacciones del módulo de aterrizaje.

Principales resultados:

Se depositaron y erosionaron finas capas (10-100s de micrómetros) de polvo rojo brillante.
La eliminación de material a escala de centímetros se produjo en áreas específicas durante una gran tormenta de polvo.
Los fuertes vientos, impulsados por las perturbaciones baroclínicas y el calentamiento de las mareas solares, estuvieron implicados en la erosión.
La erosión se concentró en áreas donde el muestreador de superficie del Viking Lander 1 había reducido la cohesión del suelo.

Conclusiones:

El material de la superficie marciana está sujeto a la redistribución por las tormentas de polvo.
La dinámica atmosférica juega un papel importante en la conducción de la erosión marciana.
Las actividades de aterrizaje pueden aumentar localmente la susceptibilidad a la erosión.
A pesar de los cambios localizados, la superficie marciana más amplia exhibe una notable estabilidad debido a la cohesión del suelo.