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Un origen de baja temperatura para los planetesimales que formaron Júpiter
T Owen1, P Mahaffy, H B Niemann
1University of Hawaii, Institute for Astronomy, Honolulu 96822, USA. owen@ifa.hawaii.edu
Nature
|December 2, 1999
Resumen
Los modelos de formación de planetas gigantes son desafiados por nuevos hallazgos. La presencia de gases nobles en Júpiter sugiere que los planetesimales se formaron a temperaturas más bajas de lo que se pensaba anteriormente, impactando las teorías de formación planetaria.
Área de la Ciencia:
- Ciencias planetarias Ciencias planetarias.
- La astroquímica es astroquímica.
- Formación del sistema solar Formación del sistema solar
Sus antecedentes:
- Los planetas gigantes exhiben mayores abundancias de elementos pesados ("metales") que el Sol.
- Los modelos actuales proponen la acreción planetesimal para explicar estos enriquecimientos.
- Se supone que los planetesimales se asemejan a los cometas modernos de la nube de Oort.
Objetivo del estudio:
- Investigar las condiciones de formación de planetesimales que contribuyeron a la composición de los planetas gigantes.
- Para conciliar las discrepancias entre las abundancias de elementos volátiles predichas y observadas en planetas gigantes.
Principales métodos:
- Análisis de las abundancias de gases nobles (argon, krypton, xenon) en la atmósfera de Júpiter.
- Comparación de las abundancias observadas con las predicciones de la composición solar y los modelos de formación.
Principales resultados:
- El argón, el criptón y el xenón están enriquecidos en la atmósfera de Júpiter de manera similar a otros elementos pesados.
- Este enriquecimiento contradice las predicciones basadas en la formación a alta temperatura de planetesimales cometarios.
Conclusiones:
- La composición de Júpiter sugiere que los planetesimales que acreció se formaron a temperaturas más bajas de las predichas por los modelos actuales de formación de planetas gigantes.
- Esto implica una revisión de los escenarios de formación para el Sistema Solar exterior y sus planetas gigantes.
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