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Una escala de masa común para los sistemas satelitales de planetas gaseosos

Robin M Canup¹, William R Ward

¹Space Studies Department, Southwest Research Institute, Boulder, Colorado 80302, USA. robin@boulder.swri.edu

|June 17, 2006

Resumen

Los planetas gigantes de nuestro Sistema Solar tienen sistemas lunares con una fracción de masa desconcertantemente pequeña. Un nuevo modelo muestra que esto está regulado por un equilibrio entre el suministro de material y la desintegración orbital impulsada por gases.

Área de la Ciencia:

Ciencias planetarias Ciencias planetarias.
La astrofísica es la astrofísica.
Formación del sistema solar Formación del sistema solar

Sus antecedentes:

Los planetas exteriores (Júpiter, Saturno, Urano) poseen muchas lunas.
Estos sistemas lunares representan una pequeña fracción consistente (aprox. 10^-4) de la masa de su planeta anfitrión.
Esta fracción de baja masa es significativamente más pequeña que la de la Luna en relación con la Tierra y ha sido un rompecabezas de larga data.

Objetivo del estudio:

Para modelar la formación y evolución de los sistemas de satélites alrededor de planetas gigantes gaseosos.
Para explicar la fracción de masa observada de los sistemas lunares alrededor de los planetas exteriores del Sistema Solar.
Investigar los procesos que regulan el crecimiento y la pérdida de satélites durante la formación de planetas.

Principales métodos:

Desarrolló un modelo numérico que simula el crecimiento y la pérdida de satélites.
Incorporó la acumulación de gas y sólidos por un planeta gigante en formación.
Analizó la interacción entre el suministro de material a los satélites y el decaimiento orbital impulsado por el disco de gas circumplanetario.

Principales resultados:

El modelo reproduce con éxito la fracción de masa observada (aprox. 10^-4) de los sistemas de satélites de Júpiter, Saturno y Urano.
Un equilibrio entre el suministro de material que entra y el decaimiento orbital del satélite impulsado por el gas regula esta fracción de masa.
El modelo sugiere que estos procesos conducen naturalmente a las propiedades observadas de los sistemas lunares de los planetas gigantes.

Conclusiones:

La fracción de masa común y baja de los sistemas de satélites de planetas gigantes es un resultado natural de los procesos de formación.
Los procesos competitivos de la acreción de satélites y el decaimiento orbital impulsado por gases son reguladores clave.
Mecanismos similares pueden limitar el tamaño de las lunas alrededor de planetas gigantes gaseosos extrasolares.

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