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Una protostar de aproximadamente 0,2 masas solares con un disco kepleriano en el muy joven sistema L1527 IRS
John J Tobin1, Lee Hartmann, Hsin-Fang Chiang
1National Radio Astronomy Observatory, Charlottesville, Virginia 22903, USA. jtobin@nrao.edu
Nature
|December 11, 2012
Resumen
Los investigadores descubrieron una relación de masa de protoestrella a envolvente significativamente más baja en el L1527 IRS, lo que indica una formación estelar en etapa temprana. Este hallazgo desafía las observaciones anteriores y proporciona nuevos conocimientos sobre los procesos de acreción protostellar.
Área de la Ciencia:
- La astronomía y la astrofísica.
- Formación estelar y evolución de las estrellas.
Sus antecedentes:
- Las protoestrellas acumulan masa de las envolturas circundantes a través de discos circumestelares durante las primeras etapas de formación.
- Anteriormente, la relación de masa más baja observada entre la protoestrella y la envolvente era de aproximadamente 2.1.
Objetivo del estudio:
- Para investigar la protoestrella L1527 IRS, que se cree que se encuentra en la fase más temprana de la formación estelar.
- Para determinar la relación de masa entre la protoestrella y la envolvente y la tasa de acreción para L1527 IRS.
Principales métodos:
- Observaciones de la emisión continua de polvo.
- Análisis de la emisión de la línea (13) CO del disco circumestelar alrededor de L1527 IRS.
Principales resultados:
- Se determinó una masa protostellar de 0,19 ± 0,04 masas solares para L1527 IRS.
- Calculó una relación de masa entre la protoestrella y la envolvente de aproximadamente 0.2, significativamente más baja que la observada anteriormente.
- Se estima una tasa de acreción de 6,6 × 10^-7 masas solares por año, lo que sugiere una edad de unos 300.000 años.
Conclusiones:
- La baja proporción de masa entre la protoestrella y la envolvente confirma que L1527 IRS se encuentra en una etapa extremadamente temprana de la formación estelar.
- La mayor parte de la luminosidad de la protoestrella se genera por acreción, con potencial para una futura adición de masa a la región de formación de planetas.
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