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Dynamic Pore-scale Reservoir-condition Imaging of Reaction in Carbonates Using Synchrotron Fast Tomography
Published on: February 21, 2017
Un origen de condensación "seco" para los carbonatos circumestelares
Alice Toppani1, François Robert, Guy Libourel
1Centre de Recherches Pétrographiques et Géochimiques-CNRS UPR 2300, 15 rue Notre Dame des Pauvres, BP 20, Vandoeuvre-les-Nancy, France. toppani2@llnl.gov
Nature
|October 21, 2005
Resumen
Los minerales carbonatados, previamente vinculados al agua, pueden formarse abiogénicamente con silicatos en el espacio. Este hallazgo sugiere nuevos orígenes para los carbonatos cósmicos en ambientes estelares calientes y densos.
Área de la Ciencia:
- La astroquímica es astroquímica.
- Ciencias planetarias Ciencias planetarias.
- La mineralogía es la Mineralogía.
Sus antecedentes:
- Los minerales carbonatados se detectan en entornos astrofísicos como las protoestrellas.
- Los carbonatos abiogénicos suelen indicar alteración acuosa con agua rica en CO2.
- Las detecciones recientes en nebulosas planetarias y protoestrellas desafían la relevancia de este indicador.
Objetivo del estudio:
- Investigar una vía de formación alternativa para los carbonatos astrofísicos.
- Explorar el papel de la condensación de no equilibrio en la formación de carbonatos.
- Comprender el origen de los carbonatos en ambientes que carecen de agua líquida.
Principales métodos:
- Simulación experimental de la condensación de no equilibrio.
- Condensación de gas de silicato en un vapor rico en H2O-CO2.
- Análisis de silicatos y carbonatos amorfos cocondensados.
Principales resultados:
- Se ha demostrado la formación abiogénica de carbonatos junto con silicatos amorfos.
- La co-condensación exitosa se produjo durante procesos de no equilibrio.
- Condiciones identificadas que favorecen la formación de carbonatos sin agua líquida.
Conclusiones:
- Los carbonatos astrofísicos pueden formarse a través de la condensación de no equilibrio en el espacio.
- Los sitios de formación propuestos incluyen vientos estelares evolucionados y flujos de salida protoestelares.
- Esto proporciona una explicación alternativa para los carbonatos cósmicos observados.
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