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Conditions on Early Earth02:06

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Los silicatos del polvo estelar provienen de meteoritos primitivos.

Kazuhide Nagashima1, Alexander N Krot, Hisayoshi Yurimoto

  • 1Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Ookayama, Meguro, Tokyo 152-8551, Japan. kazu@geo.titech.ac.jp

Nature
|May 1, 2004
PubMed
Resumen

Los granos de silicato pre-solares, anteriores a nuestro Sistema Solar, fueron descubiertos en meteoritos primitivos. Su abundancia sugiere que los silicatos eran comunes en el Sistema Solar temprano, pero probablemente fueron destruidos por el calor.

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Área de la Ciencia:

  • Cosmoquímica es la cosmoquímica.
  • Ciencias planetarias Ciencias planetarias.
  • La astronomía es la astronomía.

Sus antecedentes:

  • Los meteoritos condríticos primitivos contienen granos presolares, restos de antes de la formación de nuestro Sistema Solar.
  • Se espera que los silicatos sean sólidos dominantes en los discos protoplanetarios, sin embargo, no se han encontrado silicatos presolares en las condritas.

Objetivo del estudio:

  • Para informar sobre el descubrimiento in situ de granos de silicato presolar en condritas carbonáceas primitivas.
  • Para investigar el origen y la abundancia de estos silicatos presolares.

Principales métodos:

  • Análisis in situ de granos de silicato presolar (0,1-1 micrómetros) dentro de las matrices de los meteoritos.
  • Análisis isotópico de oxígeno y silicio en los granos descubiertos.

Principales resultados:

  • Descubrimiento de granos de silicato presolar en dos condritas carbonáceas primitivas.
  • Los granos muestran un alto enriquecimiento de 17O (delta17O(SMOW) > 100-400 por mil) y una composición isotópica de silicio solar.
  • Abundancia estimada de 3-30 partes por millón, más alta que otros granos presolares pero más baja que en las partículas de polvo interplanetario.

Conclusiones:

  • Los silicatos presolares probablemente se originaron en estrellas gigantes rojas ricas en oxígeno o en estrellas gigantes asintóticas.
  • La menor abundancia en los meteoritos en comparación con las partículas de polvo interplanetario sugiere la destrucción de silicatos durante el procesamiento a alta temperatura en la nebulosa solar.