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Simulation of the Planetary Interior Differentiation Processes in the Laboratory
Published on: November 15, 2013
El surgimiento de dos tipos de planetas terrestres en la solidificación del magma oceánico
Keiko Hamano1, Yutaka Abe, Hidenori Genda
1Department of Earth and Planetary Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan. keiko@eps.s.u-tokyo.ac.jp
Nature
|May 31, 2013
Resumen
Los planetas terrestres se forman en dos tipos basados en la solidificación de un estado fundido. Los planetas tipo I retienen agua para los océanos, mientras que los planetas tipo II pierden agua debido a los océanos de magma prolongados y el escape hidrodinámico.
Área de la Ciencia:
- Ciencias planetarias Ciencias planetarias.
- Ciencias de la Tierra Ciencias de la Tierra Ciencias de la Tierra
- La astrofísica es la astrofísica.
Sus antecedentes:
- Comprender la diversidad de los planetas terrestres es clave en las ciencias planetarias.
- Venus, similar a la Tierra, carece de agua, lo que pone de relieve una brecha en los modelos de evolución planetaria.
- La predicción de las atmósferas de los exoplanetas requiere un marco general para la evolución planetaria.
Objetivo del estudio:
- Establecer un marco para la evolución planetaria basado en procesos de solidificación.
- Para clasificar los planetas terrestres en tipos distintos basados en su formación y evolución.
- Para explicar la divergencia en el contenido de agua planetaria, usando a Venus como un estudio de caso.
Principales métodos:
- Análisis de la solidificación planetaria desde un estado fundido inicialmente caliente.
- Modelado de la evolución planetaria teniendo en cuenta factores como la distancia de la estrella anfitriona y el contenido de agua.
- Clasificación de los planetas en Tipo I y Tipo II basada en la duración de la solidificación y la retención de agua.
Principales resultados:
- Los planetas terrestres se solidifican en dos tipos distintos: Tipo I (formado más allá de una distancia crítica) y Tipo II (formado dentro de una distancia crítica).
- Los planetas de tipo I se solidifican rápidamente, reteniendo agua para formar los primeros océanos.
- Los planetas de tipo II experimentan océanos de magma prolongados (hasta 100 millones de años), lo que lleva a la desecación a través del escape hidrodinámico, consistente con las características de Venus.
Conclusiones:
- Las vías evolutivas planetarias divergen significativamente incluso para planetas con condiciones iniciales similares.
- La clasificación Tipo I/Tipo II proporciona un marco para comprender la distribución del agua en los planetas terrestres.
- Las futuras observaciones pueden detectar planetas oceánicos ricos en agua y magma alrededor de estrellas jóvenes.
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