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Cambio en la composición química del gas que cae formando un disco alrededor de una protoestrella

Nami Sakai¹, Takeshi Sakai², Tomoya Hirota³

¹Department of Physics, The University of Tokyo, Hongo, Bunkyo-ku, Tokyo 113-0033, Japan.

|February 14, 2014

Resumen

Los investigadores descubrieron distintas composiciones químicas en la envoltura y la barrera centrífuga de una joven protoestrella, IRAS 04368+2557. El C3H2 cíclico se encuentra en el sobre, mientras que el monóxido de azufre (SO) se mejora en la barrera centrífuga, revelando nuevos conocimientos sobre la química de la formación estelar.

Área de la Ciencia:

* Astronomía y astrofísica.
* Astroquímica es la astroquímica.
* Formación Estelar Formación Estelar

Sus antecedentes:

* IRAS 04368+2557 es una protoestrella cercana de baja masa en la nube molecular de Tauro, que sirve como un sitio clave para estudiar la formación de estrellas y sistemas planetarios.
* La envoltura protostellar se caracteriza por la caída y rotación de gas, con un aumento significativo de la densidad y la temperatura hacia el disco protostellar.
* Los estudios anteriores carecían de una comprensión detallada de los cambios en la composición química durante el colapso de la envoltura al disco.

Objetivo del estudio:

* Para investigar la composición química de la envoltura en caída y la zona de transición de la protoestrella IRAS 04368+2557.7.
* Explorar cómo los cambios químicos se correlacionan con procesos físicos como la caída y rotación de gases.

Principales métodos:

* Observación de la protoestrella IRAS 04368+2557 utilizando instrumentos astronómicos avanzados (detalles no especificados en el resumen).
* Análisis de la emisión de líneas moleculares para identificar y mapear la distribución de moléculas específicas dentro del sistema protostellar.

Principales resultados:

* Se detectó la molécula insaturada de hidrocarburos cíclica-C3H2 en el sobre giratorio que cae hacia abajo.
* Se encontró que el monóxido de azufre (SO) estaba significativamente mejorado en la zona de transición en la barrera centrífuga (radio de ~ 100 UA).
* Esta diferenciación química en la barrera centrífuga fue inesperada.

Conclusiones:

* La segregación química observada sugiere condiciones físicas y procesos distintos en diferentes radios dentro del sistema protostellar.
* El aumento de SO en la barrera centrífuga puede estar relacionado con el movimiento de caída discontinuo y el calentamiento local.
* Estos hallazgos proporcionan nuevos conocimientos sobre la química compleja que rige las primeras etapas de la formación de estrellas y planetas.

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