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Evidencia de un disco de acreción del tamaño del sistema solar alrededor de la masiva protoestrella G192.16-3.822
D S Shepherd1, M J Claussen, S E Kurtz
1National Radio Astronomy Observatory, Post Office Box 0, Socorro, NM 87801, USA. dshepher@aoc.nrao.edu
Science (New York, N.Y.)
|May 26, 2001
Resumen
Los astrónomos encontraron un disco de acreción del tamaño de un sistema solar alrededor de una protoestrella masiva, G192 S1, lo que sugiere un sistema protostellar binario. Este descubrimiento ofrece nuevos conocimientos sobre la formación y evolución de estrellas masivas.
Área de la Ciencia:
- La radioastronomía es una radioastronomía.
- La astrofísica es la astrofísica.
- Formación Estelar Formación Estelar.
Sus antecedentes:
- Las estrellas masivas son cruciales para la evolución galáctica.
- Comprender su formación es clave para la astrofísica.
- Las limitaciones observacionales en las protoestrellas masivas son limitadas.
Objetivo del estudio:
- Para investigar la estructura de la fuente de salida bipolar masiva G192.16-3.82.82.
- Para buscar evidencia de un disco de acreción alrededor de una protoestrella masiva.
- Para modelar la emisión de radio para comprender el sistema protostellar.
Principales métodos:
- Utilizó el Very Long Baseline Array (VLBA) y el Very Large Array (VLA) para observaciones de radio de alta resolución.
- Realizó observaciones en el continuo de siete milímetros.
- Desarrolló un modelo de la emisión de radio.
Principales resultados:
- Se resolvió un disco de acreción del tamaño del sistema solar (130 UA de diámetro) alrededor de la protoestrella primaria (G192 S1).
- Se estimó la masa de la protoestrella en 8-10 masas solares.
- Identificó una fuente compañera (G192 S2) 80 UA al norte de la primaria.
- Caracterizó el flujo de salida como poco colimado (ángulo de apertura de 40 grados).
Conclusiones:
- Los hallazgos proporcionan una fuerte evidencia de un verdadero disco de acreción alrededor de una protoestrella masiva.
- Los resultados sugieren que G192.16-3.82 es un sistema protostellar binario.
- El estudio avanza nuestra comprensión de los procesos de acreción en la formación de estrellas masivas.
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