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Una importante trampa de polvo asimétrica en un disco de transición
Nienke van der Marel1, Ewine F van Dishoeck, Simon Bruderer
1Leiden Observatory, Leiden University, Leiden, Netherlands. nmarel@strw.leidenuniv.nl
Science (New York, N.Y.)
|June 8, 2013
Resumen
Los astrónomos detectaron una trampa de polvo en el disco protoplanetario Oph IRS 48 utilizando las observaciones de Atacama Large Millimeter/submillimeter Array (ALMA). Este hallazgo apoya las teorías de que las trampas de polvo ayudan a superar la deriva de partículas durante la formación de planetas.
Área de la Ciencia:
- * La astronomía es la astronomía.
- * Astrofísica es la astrofísica.
- * Ciencias planetarias Ciencias planetarias
Sus antecedentes:
- * Las teorías de formación planetaria se enfrentan a desafíos, incluida la deriva hacia el interior de las partículas en los discos protoplanetarios.
- * Se supone que las trampas de polvo resuelven estos problemas concentrando partículas.
- * La comprensión de la distribución del polvo es crucial para explicar la eficiencia de la formación de planetas.
Objetivo del estudio:
- * Detectar y caracterizar una trampa de polvo en el disco protoplanetario de Oph IRS 48.
- * Para investigar la distribución de diferentes tamaños de granos de polvo y gas dentro del disco.
- * Para probar modelos teóricos de la formación de trampas de polvo, en particular trampas inducidas por vórtices.
Principales métodos:
- * Utilizó el Atacama Large Millimeter/submillimeter Array (ALMA) para observaciones de alta resolución.
- * Analizó la emisión continua de 0,44 milímetros para mapear los grandes granos de polvo.
- * Comparación de la distribución del polvo con imágenes de infrarrojo medio (pequeño polvo) y observaciones de monóxido de carbono (gas).
Principales resultados:
- * Se detectó una clara trampa de polvo en forma de media luna rica en granos de tamaño milimétrico en un lado de Oph IRS 48.
- * Se observó que las partículas de polvo y gas más pequeñas se concentran centralmente en anillos, en contraste con los granos más grandes.
- * La separación espacial observada entre el polvo/gas grande y pequeño es consistente con los modelos de una trampa de polvo inducida por vórtices.
Conclusiones:
- * La detección de una trampa de polvo en Oph IRS 48 proporciona evidencia observacional que apoya las teorías de la trampa de polvo en la formación de planetas.
- * Los hallazgos sugieren que un vórtice inducido por un compañero puede ser responsable de crear esta trampa de polvo.
- * Este descubrimiento ofrece información sobre los mecanismos que facilitan la formación planetesimal mediante la concentración de polvo.
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