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Un disco de polvo y gas molecular alrededor de una protoestrella de gran masa
Nimesh A Patel1, Salvador Curiel, T K Sridharan
1Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS78, Cambridge, Massachusetts 02138, USA.
Nature
|September 2, 2005
Resumen
La formación de estrellas de alta masa puede ocurrir a través de la acreción, similar a las estrellas de baja masa. Las observaciones revelan un disco alrededor de una protoestrella masiva, apoyando este modelo de acreción para el nacimiento de estrellas masivas.
Área de la Ciencia:
- La astrofísica es la astrofísica.
- Evolución Estelar Evolución Estelar
Sus antecedentes:
- La formación de estrellas de baja masa se entiende bien.
- Los mecanismos de formación de estrellas de alta masa siguen siendo poco conocidos.
- La acreción frente a las fusiones estelares es un debate clave en la formación de estrellas de alta masa.
Objetivo del estudio:
- Para investigar el proceso de formación de estrellas de alta masa.
- Para determinar si las estrellas de alta masa se forman a través de la acreción de discos circumestelares.
- Para proporcionar evidencia a favor o en contra del modelo de acreción en la formación de estrellas de alta masa.
Principales métodos:
- Astronomía observacional centrada en la emisión continua de polvo.
- Análisis de la emisión de la línea de gas molecular.
- Observaciones por radio de los chorros bipolares.
Principales resultados:
- Detección de una estructura aplanada en forma de disco alrededor de una protoestrella de 15 masas solares.
- El disco tiene un radio de aproximadamente 330 unidades astronómicas y una masa de 1-8 masas solares.
- El disco está orientado perpendicularmente al chorro de radio bipolar observado.
Conclusiones:
- Las estrellas de alta masa pueden formarse a través de la acreción.
- La estructura del disco observada apoya la acreción como un mecanismo de formación de estrellas masivas.
- Los hallazgos alinean los procesos de formación de estrellas de baja y alta masa.
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