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Detección del depósito de agua en un sistema planetario en formación
Michiel R Hogerheijde1, Edwin A Bergin, Christian Brinch
1Leiden Observatory, Leiden University, Post Office Box 9513, 2300 RA Leiden, Netherlands. michiel@strw.leidenuniv.nl
Science (New York, N.Y.)
|October 25, 2011
Resumen
Vapor de agua fría detectado en una estrella joven.
Área de la Ciencia:
- La astronomía y la astrofísica.
- Ciencias planetarias Ciencias planetarias.
- La astroquímica es astroquímica.
Sus antecedentes:
- Se supone que el origen de los océanos de la Tierra son cuerpos helados, pero el agua en los discos de formación de planetas extrasolares sigue siendo poco comprendida.
- El vapor de agua fría es crucial para comprender la formación de planetas y el potencial de entornos habitables más allá de nuestro sistema solar.
Objetivo del estudio:
- Para investigar la presencia y el origen del vapor de agua fría en el disco de la joven estrella TW Hydrae.
- Para determinar la masa del reservorio de hielo de agua y su relación orto-para en un disco protoplanetario extrasolar.
Principales métodos:
- Utilizó el instrumento heterodino para el infrarrojo lejano (HIFI) a bordo del Observatorio Espacial Herschel.
- Se detectaron líneas de emisión de ambos isómeros de espín del vapor de agua fría (H2O).
Principales resultados:
- Se confirmó la presencia de vapor de agua fría en el disco de TW Hydrae.
- Se estima un depósito sustancial de hielo de agua, potencialmente miles de veces la masa de los océanos de la Tierra.
- Se midió una relación orto-para significativamente menor que la encontrada en los cometas del sistema solar.
Conclusiones:
- El vapor de agua detectado probablemente se origina en sólidos cubiertos de hielo en la superficie del disco.
- La baja relación orto-para sugiere que los cometas se forman a partir de mezclas heterogéneas de hielo formadas en toda la nebulosa solar.
- Este hallazgo proporciona información sobre las primeras etapas del nacimiento planetario y los mecanismos de suministro de agua.
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