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Partición isotópica de oxígeno independiente de la masa durante la formación de SiO2 en fase gaseosa

Subrata Chakraborty¹, Petia Yanchulova, Mark H Thiemens

¹Department of Chemistry and Biochemistry, University of California, San Diego, La Jolla, CA 92093-0356, USA.

Science (New York, N.Y.)

|October 26, 2013

Resumen

Los científicos demostraron experimentalmente una reacción química independiente de la masa durante la oxidación del monóxido de silicio. Este proceso podría explicar las diversas composiciones de isótopos de oxígeno que se encuentran en los meteoritos, arrojando luz sobre las primeras condiciones de la nebulosa solar.

Área de la Ciencia:

Ciencias planetarias Ciencias planetarias.
La geoquímica es la geoquímica.
La astroquímica es astroquímica.

Sus antecedentes:

Los meteoritos exhiben diversas composiciones isotópicas de oxígeno, lo que sugiere heterogeneidad en la nebulosa solar temprana.
Las composiciones isotópicas anómalas en los minerales refractarios de meteoritos pueden surgir de la fraccionamiento químico nebular, pero falta evidencia experimental.

Objetivo del estudio:

Investigar experimentalmente los procesos de conversión de gas en partículas relevantes para la formación de meteoritos.
Para determinar si las reacciones químicas en la nebulosa pueden producir fraccionamientos de isótopos de oxígeno independientes de la masa.

Principales métodos:

Oxidación experimental del gas de monóxido de silicio (SiO).
Análisis de las proporciones de isótopos de oxígeno ((18) O / ((16) O y (17) O / ((16) O) en las partículas resultantes.

Principales resultados:

Se observó una línea independiente de la masa con una pendiente de uno en el espacio de tres isótopos de oxígeno.
Demostró que la oxidación en fase gaseosa del SiO puede producir composiciones isotópicas anómalas de oxígeno.

Conclusiones:

La reacción estudiada es un paso inicial potencial para la producción de reservas anómalas de isótopos de oxígeno en la nebulosa solar.
Este hallazgo experimental apoya la fraccionamiento químico como un mecanismo para la heterogeneidad isotópica del meteorito.

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