Formación episódica de material cometario en el estallido de una joven estrella similar al Sol
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Laboratory Drop Towers for the Experimental Simulation of Dust-aggregate Collisions in the Early Solar System
Published on: June 5, 2014
P Abrahám1, A Juhász, C P Dullemond
1Konkoly Observatory of the Hungarian Academy of Sciences, PO Box 67, 1525 Budapest, Hungary. abraham@konkoly.hu
Nature
|May 16, 2009
Resumen
El polvo cristalino en los sistemas estelares jóvenes se forma a través del recocido térmico durante las explosiones estelares, no el calentamiento por choque. Este hallazgo aclara el sistema solar temprano.
Área de la Ciencia:
- Ciencias planetarias Ciencias planetarias.
- La astrofísica es la astrofísica.
- Cosmoquímica es la cosmoquímica.
Sus antecedentes:
- El Sistema Solar se formó a partir de gas y polvo interestelar, inicialmente silicato amorfo y partículas carbonáceas.
- El material cometario indica una transformación significativa de silicatos amorfos en formas cristalinas durante la evolución de la nebulosa protosolar.
- El momento y el mecanismo (calentamiento solar vs. calentamiento por choque) de esta transformación de silicato siguen siendo objeto de debate.
Objetivo del estudio:
- Para investigar el proceso de formación de silicatos cristalinos en los discos protoplanetarios.
- Determinar el papel de la actividad estelar, específicamente los estallidos, en el procesamiento del polvo.
- Diferenciar entre el calentamiento solar y el calentamiento por choque como mecanismos para la cristalización del silicato.
Principales métodos:
- Observación de las características espectrales del infrarrojo medio de la joven estrella similar al Sol EX Lupi durante las fases de quiescencia y estallido.
- Análisis de datos espectrales para identificar la presencia y composición de partículas de polvo.
- Comparación de las características observadas con modelos teóricos de procesamiento de polvo bajo diferentes escenarios de calentamiento.
Principales resultados:
- Se detectaron nuevas características espectrales en el infrarrojo medio, atribuidas a la forsterita cristalina, durante el estallido de EX Lupi, pero no durante la quiescencia.
- El forsterito cristalino observado indica la formación a través del recocido térmico.
- La ausencia de cristales fríos en el espectro observado descarta el calentamiento por choque en radios de disco más grandes.
Conclusiones:
- Las explosiones estelares proporcionan suficiente energía térmica para recocer silicatos amorfos en formas cristalinas en las capas internas de la superficie del disco.
- El recocido térmico durante los estallidos es un mecanismo previamente no considerado pero significativo para la producción de polvo cristalino.
- Es poco probable que el calentamiento por choque sea el mecanismo principal para la generalización de la cristalización de silicatos en el Sistema Solar temprano.
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