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Olivina de supernova obtenida del polvo cometario.

Scott Messenger1, Lindsay P Keller, Dante S Lauretta

  • 1Mail Code KR, Robert M. Walker Laboratory for Space Science, NASA Johnson Space Center, Houston, TX 77058, USA. scott.r.messenger@nasa.gov

Science (New York, N.Y.)
|July 5, 2005
PubMed
Resumen

Un grano de polvo presolar de una supernova revela firmas isotópicas únicas. Esta partícula interplanetaria ofrece pistas sobre la nucleosíntesis estelar y la formación temprana del sistema solar.

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Área de la Ciencia:

  • Cosmoquímica es la cosmoquímica.
  • Astrogeología y Astrogeología.
  • Ciencias planetarias Ciencias planetarias.

Sus antecedentes:

  • Las partículas de polvo interplanetario (IDP) son fragmentos microscópicos extraterrestres que se encuentran en la Tierra.
  • El estudio de sus composiciones isotópicas puede revelar sus orígenes en estrellas y supernovas.
  • Los granos presolares proporcionan evidencia directa de procesos nucleosintéticos más allá de nuestro sistema solar.

Objetivo del estudio:

  • Para analizar la composición isotópica y las microestructuras de una partícula específica de polvo interplanetario.
  • Para determinar el origen y las condiciones de formación del grano de polvo.
  • Para investigar el vínculo potencial entre las eyecciones de supernovas y la materia orgánica presolar.

Principales métodos:

  • Análisis isotópico de oxígeno (18O/16O, 17O/16O) y silicio (29Si/28Si).
  • Examen microestructural del agregado de silicato cristalino.
  • Identificación de las fases minerales, específicamente el olivino.

Principales resultados:

  • El grano de polvo exhibe un enriquecimiento significativo en 18O/16O y agotamientos en 17O/16O y 29Si/28Si.
  • Estas anomalías isotópicas son consistentes con la formación de una supernova de tipo II.
  • El grano contiene olivina forsterita submicrometrica con mínima alteración térmica, envuelta en materia orgánica rica en nitrógeno-15.

Conclusiones:

  • El grano analizado es probablemente un silicato presolar formado en una supernova.
  • Su composición sugiere la formación a través de la condensación de equilibrio de zonas nucleosintéticas mixtas en las eyecciones de supernovas.
  • La materia orgánica asociada probablemente se formó en una nube molecular fría presolar, lo que indica un origen complejo para los primeros materiales del sistema solar.