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Simulation of the Planetary Interior Differentiation Processes in the Laboratory

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Composición de la superficie de Hiperión

D P Cruikshank¹, J B Dalton, C M Dalle Ore

¹NASA Ames Research Center, MS 245-6, NASA Ames Research Center, MS 211-3, Moffett Field, California 94035, USA. Dale.P.Cruikshank@nasa.gov

|July 6, 2007

Resumen

Este resumen es generado por máquina.

La luna de Saturno Hiperión tiene dos materiales de superficie distintos. El material de bajo albedo en los cráteres comparte similitudes espectrales con las lunas de Saturno Phoebe e Iapetus.

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Área de la Ciencia:

Ciencias planetarias Ciencias planetarias.
Astrogeología y Astrogeología.
La espectroscopia es una técnica de espectroscopia.

Sus antecedentes:

Hiperión es la octava luna más grande de Saturno, caracterizada por una forma irregular y una rotación caótica.
Su superficie exhibe dos unidades principales: un componente de alto albedo rico en hielo de agua y un componente de bajo albedo encontrado en cráteres.

Objetivo del estudio:

Para analizar las propiedades espectrales de los componentes de la superficie de Hyperion en las regiones ultravioleta e infrarroja cercana.
Para identificar la composición y los posibles orígenes del material de bajo albedo en Hyperion.

Principales métodos:

Utilizó dos instrumentos ópticos de teledetección a bordo de la nave espacial Cassini.
Espectro de reflexión adquirido de la superficie de Hiperión durante un sobrevuelo cercano el 25 y 26 de septiembre de 2005.

Principales resultados:

Se obtuvieron distintos espectros ultravioleta e infrarrojo cercano para materiales de superficie de alto y bajo albedo.
El material de bajo albedo muestra similitudes espectrales con la superficie de Febe e Iapetus.

Conclusiones:

El material de bajo albedo en Hyperion puede compartir un origen común o estar relacionado con los materiales encontrados en Phoebe e Iapetus.
Se justifica una mayor investigación sobre los vínculos de composición entre estas lunas de Saturno.