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Imagen de la línea de nieve de CO en una nebulosa solar analógica
Chunhua Qi1, Karin I Öberg, David J Wilner
1Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA. cqi@cfa.harvard.edu
Science (New York, N.Y.)
|July 23, 2013
Resumen
Los astrónomos mapearon la línea de nieve de monóxido de carbono (CO) en el disco TW Hya utilizando observaciones de Atacama Large Millimeter/Submillimeter Array. Esto proporciona datos cruciales para comprender la formación de planetas y la dinámica del sistema solar.
Área de la Ciencia:
- Ciencias planetarias Ciencias planetarias.
- La astronomía es la astronomía.
- La astroquímica es astroquímica.
Sus antecedentes:
- Los planetas se forman en discos protoplanetarios alrededor de estrellas jóvenes.
- La composición y la eficiencia de formación de los planetas dependen de la ubicación de las líneas de nieve volátil dentro de estos discos.
Objetivo del estudio:
- Para obtener imágenes químicas de la línea de nieve de monóxido de carbono (CO) en el disco protoplanetario que rodea a TW Hya.
- Utilizar estos datos para evaluar modelos de la dinámica de formación del sistema solar.
Principales métodos:
- Utilizó observaciones de Atacama Large Millimeter/Submillimeter Array (ALMA) de alta resolución espacial y espectral.
- Se detectó la emisión de diazenilium (N2H(+), un marcador para las regiones donde el CO está congelado.
Principales resultados:
- Se presenta una imagen química de la línea de nieve de CO en el disco TW Hya.
- La emisión observada de N2H ((+) forma un gran anillo, indicando la ubicación de la línea de nieve.
- Determinó que el radio de la línea de nieve de CO es de aproximadamente 30 unidades astronómicas.
Conclusiones:
- El radio de la línea de nieve de CO observado en TW Hya se alinea con las predicciones del modelo.
- Este hallazgo ayuda a evaluar los modelos de la dinámica de formación del sistema solar.
- Los resultados se pueden combinar con datos de composición planetaria y cometaria para obtener más información.
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