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La composición isotópica de oxígeno del Sol se infiere a partir del viento solar capturado
K D McKeegan1, A P A Kallio, V S Heber
1Department of Earth and Space Sciences, University of California-Los Angeles (UCLA), Los Angeles, CA 90095-1567, USA. mckeegan@ess.ucla.edu
Science (New York, N.Y.)
|June 25, 2011
Resumen
El Sol tiene una mayor abundancia de oxígeno-16 (16O) que los materiales rocosos del sistema solar interior. Esto sugiere que la química temprana no dependiente de la masa enriqueció los planetas terrestres en isótopos de oxígeno más pesados.
Área de la Ciencia:
- Cosmoquímica es la cosmoquímica.
- Ciencias planetarias Ciencias planetarias.
- Astrobiología Astrobiología.
Sus antecedentes:
- Las composiciones de isótopos de oxígeno de los materiales del sistema solar han mostrado variaciones significativas.
- No se ha establecido una composición definitiva de isótopos de oxígeno del sistema solar primordial.
- La fotosfera del Sol se considera representativa de la composición isotópica promedio del sistema solar para elementos más pesados que el litio.
Objetivo del estudio:
- Para determinar la composición isotópica de oxígeno del Sol.
- Para comparar los isótopos de oxígeno del Sol con los de los materiales planetarios del sistema solar interior.
- Para investigar el origen de las variaciones isotópicas en el sistema solar interior.
Principales métodos:
- Análisis de muestras de viento solar devueltas a la Tierra por la misión Genesis de la NASA.
- Medición de las relaciones isotópicas de oxígeno ((16) O, (17) O, (18) O) en el viento solar.
- Comparación de los datos isotópicos del viento solar con los datos existentes para la Tierra, la Luna, Marte y los meteoritos.
Principales resultados:
- El Sol exhibe un enriquecimiento significativo en oxígeno-16 (16O) en comparación con la Tierra, la Luna, Marte y los meteoritos a granel.
- Los cuerpos rocosos del sistema solar interno están agotados en 16O en relación con el Sol.
- Estos hallazgos implican que los materiales rocosos están enriquecidos en isótopos de oxígeno más pesados ((17) O y (18) O) en aproximadamente un 7% en relación con 16O.
Conclusiones:
- La composición isotópica del Sol refleja el promedio para el sistema solar temprano.
- Los materiales rocosos en el interior del sistema solar probablemente sufrieron enriquecimiento en 17O y 18O.
- Este enriquecimiento probablemente fue el resultado de procesos químicos no dependientes de la masa que ocurrieron antes de la acreción planetesimal.
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