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Hierro vivo-60 en el sistema solar temprano
Science (New York, N.Y.)
|February 19, 1993
Resumen
El hierro-60 (Fe-60) de corta duración estuvo presente en el sistema solar temprano, como lo demuestra el exceso de níquel-60 (Ni-60) en el meteorito Chervony Kut. Su descomposición probablemente proporcionó calor para la fusión de los primeros cuerpos planetarios.
Área de la Ciencia:
- Cosmoquímica es la cosmoquímica.
- Ciencias planetarias Ciencias planetarias.
- La astrofísica nuclear es una astrofísica nuclear.
Sus antecedentes:
- El sistema solar primitivo era un entorno dinámico con isótopos radiactivos de corta duración.
- Comprender la distribución y el impacto de estos isótopos es crucial para los modelos de formación planetaria.
Objetivo del estudio:
- Investigar la presencia e implicaciones del extinto radionucleido hierro-60 (Fe-60) en el sistema solar temprano.
- Determinar si el decaimiento del Fe-60 contribuyó a la evolución térmica de los planetesimales.
Principales métodos:
- Análisis isotópico del níquel (Ni) en muestras del meteorito Chervony Kut.
- Cuantificación de los excesos relativos de Ni-60 atribuidos a la desintegración del Fe-60.
Principales resultados:
- Se observaron excesos de Ni-60 que oscilaban entre 2,4 y 50 partes por 10^4 en muestras de meteoritos.
- Evidencia de la presencia de Fe-60 durante la fusión / diferenciación y la solidificación magmática posterior.
- Abundancia inferida de Fe-60 suficiente para derretir pequeños cuerpos planetarios.
Conclusiones:
- El Fe-60 extinto estaba presente en grandes escalas en el sistema solar temprano.
- La desintegración del Fe-60 fue una fuente de calor significativa para la fusión y diferenciación de los primeros planetesimales.
- Esto proporciona información sobre la historia térmica y la formación de planetas terrestres.
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