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La estrella compañera binaria masiva del progenitor de la supernova 1993J
Justyn R Maund1, Stephen J Smartt, Rolf P Kudritzki
1Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK. jrm@ast.cam.ac.uk
Nature
|January 9, 2004
Resumen
Diez años después de la supernova SN1993J, los astrónomos detectaron su estrella compañera binaria masiva. Este descubrimiento confirma que la estrella progenitora perdió su envoltura de hidrógeno por esta compañera, lo que explica la supernova.
Área de la Ciencia:
- La astronomía y la astrofísica.
- Evolución Estelar Evolución Estelar
- Las supernovas son las supernovas.
Sus antecedentes:
- Supernova (SN) 1993J, inicialmente clasificada como Tipo II rica en hidrógeno, se transformó en un Tipo Ib deficiente en hidrógeno.
- Las observaciones previas a la explosión sugirieron que el progenitor de SN 1993J era una supergigante roja con una compañera masiva o en una asociación estelar joven.
- Los modelos propusieron que SN 1993J era una supernova de tipo IIb, resultado de la transferencia de masa a un compañero binario, pero este compañero permaneció sin ser descubierto.
Objetivo del estudio:
- Para identificar la escurridiza estrella compañera masiva de la progenitora de la supernova (SN) 1993J.
- Confirmar el papel del compañero binario en el proceso de pérdida de masa que conduce a la evolución espectral única de SN 1993J.
- Proporcionar evidencia observacional para la hipótesis de la compañera binaria en las supernovas de tipo IIb.
Principales métodos:
- Se realizaron observaciones fotométricas y espectroscópicas de SN 1993J diez años después de la explosión.
- Analizaron datos para detectar y caracterizar las firmas estelares en la ubicación de la supernova.
- Utilizó técnicas avanzadas de imagen para resolver objetos débiles cerca del remanente de supernova.
Principales resultados:
- Detectó la firma inequívoca de una estrella masiva en el sitio de la supernova desvanecida SN 1993J.
- Confirmó la presencia de la estrella compañera binaria del progenitor de la supernova.
- La estrella compañera detectada proporciona evidencia directa para el modelo de interacción binaria.
Conclusiones:
- La estrella masiva detectada es la compañera binaria responsable de despojar la envoltura de hidrógeno del progenitor.
- Este descubrimiento proporciona la primera evidencia directa de la existencia de estrellas compañeras masivas en los progenitores de supernovas Tipo IIb.
- Los hallazgos resuelven un misterio de larga data con respecto a la naturaleza de SN 1993J y su sistema progenitor.
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