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Ventanas a través de los discos polvorientos que rodean a los objetos protoestelares más jóvenes de baja masa
J Cernicharo1, A Noriega-Crespo, D Cesarsky
1Consejo Superior de Investigaciones Científicas, Instituto de Estructura de la Materia, Departamento Física Molecular, Serrano 121, 28006 Madrid, Spain. cerni@astro.iem.csic.es
Science (New York, N.Y.)
|April 28, 2000
Resumen
Detectamos la emisión de infrarrojo medio (IR medio) de la joven protoestrella VLA1 utilizando el Observatorio Espacial Infrarrojo. Esto revela las regiones más internas de las protoestrellas, previamente ocultas por discos oscuros.
Área de la Ciencia:
- La astronomía y la astrofísica.
- Evolución Estelar Evolución Estelar
- Astronomía por infrarrojos Astronomía por infrarrojos
Sus antecedentes:
- La formación de estrellas jóvenes de baja masa implica acreción y pérdida de masa en los discos circumestelares.
- Las protoestrellas de clase 0 están fuertemente oscurecidas en longitudes de onda ópticas e infrarrojas, lo que dificulta la observación.
- La interferometría de radio fue el método principal para detectar estas protostarras ocultas en etapa temprana.
Objetivo del estudio:
- Para detectar la emisión de infrarrojo medio (IR medio) de la protoestrella de clase 0 VLA1.1.
- Para investigar las regiones más interiores de jóvenes protoestrellas previamente ocultas por discos circumestelares.
- Para utilizar ventanas específicas de longitud de onda de infrarrojos medios con una absorción mínima por hielo y silicatos.
Principales métodos:
- Utilizó el Observatorio Espacial Infrarrojo (ISO) para observaciones en el infrarrojo medio.
- Centrado en ventanas de longitud de onda (5.3, 6.6 y 7.5 micrómetros) con baja absorción interestelar.
- Emisión analizada de la región HH1-HH2 en la Nebulosa de Orión.
Principales resultados:
- Se ha detectado con éxito la emisión infrarroja media de la protoestrella de clase 0 VLA1.1.
- La emisión se origina en una fuente central compacta (aprox. 4 UA de diámetro) con una temperatura de ~700 K.
- La protoestrella está profundamente incrustada dentro de una región de alta extinción visual (80-100 magnitudes).
Conclusiones:
- Las observaciones en el infrarrojo medio pueden sondear las regiones interiores oscurecidas de las protoestrellas jóvenes.
- La emisión detectada proporciona información sobre las condiciones físicas del sistema protostellar más interno.
- Este método abre nuevas vías para el estudio de las primeras etapas de la evolución estelar anteriormente inaccesibles.
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