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La fusión planetesimal temprana desde una edad de 4.5662 Gyr para meteoritos diferenciados
Joel Baker1, Martin Bizzarro, Nadine Wittig
1School of Earth Sciences, Victoria University of Wellington, PO Box 600, Wellington, New Zealand. joel.baker@vuw.ac.nz
Nature
|August 27, 2005
Resumen
Los isótopos radiactivos en los meteoritos ayudan a datar la formación del Sistema Solar. Los meteoritos de angrita, fechados hace 4.5662 mil millones de años, confirman que los isótopos de corta duración desencadenaron el derretimiento temprano de los planetesimales.
Área de la Ciencia:
- Cosmoquímica es la cosmoquímica.
- Ciencias planetarias Ciencias planetarias.
- Geocronología Geocronología.
Sus antecedentes:
- Los isótopos radiactivos en los meteoritos sirven como cronómetros para los modelos de formación del Sistema Solar.
- Los meteoritos diferenciados se originan a partir de cuerpos madre fundidos, sin embargo, sus edades minerales son a menudo más jóvenes que las líneas de tiempo de diferenciación.
- Las edades más jóvenes sugieren fuentes de calor como núcleos de corta vida ((26) Al, (60) Fe) que se desintegran antes de fundirse, desafiando los modelos existentes.
Objetivo del estudio:
- Para investigar el momento de la fusión planetesimal y su fuente de calor.
- Para refinar la edad mínima del Sistema Solar utilizando la datación por meteoritos de angrita.
- Para probar el papel de los nucleidos radiactivos de corta duración en los primeros eventos térmicos del Sistema Solar.
Principales métodos:
- Datamiento plomo-plomo (Pb-Pb) de las angritas basálticas.
- Medición de excesos de magnesio-26 ((26) Mg) en muestras masivas de angrita.
Principales resultados:
- Las angritas basálticas datan de hace 4.5662 ± 0.0001 mil millones de años, solo 1 millón de años más jóvenes que la edad mínima del Sistema Solar.
- Confirmación de que la desintegración de (26) Al contribuyó a la fusión del cuerpo madre de la angrita a través de los excesos de (26) Mg observados.
- La edad mínima revisada del Sistema Solar es de 4.5695 ± 0.0002 mil millones de años.
Conclusiones:
- La acumulación de planetesimales diferenciados probablemente precedió a los planetesimales indiferenciados.
- Los nucleidos de corta duración, específicamente (26) Al y (60) Fe, fueron capaces de desencadenar el derretimiento planetesimal poco después de su inyección.
- El estudio refina nuestra comprensión de la historia térmica y la edad del Sistema Solar temprano.
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