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Un tipo débil de supernova de una enana blanca con una compañera rica en helio
H B Perets1, A Gal-Yam, P A Mazzali
1Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel. hperets@cfa.harvard.edu
Nature
|May 21, 2010
Resumen
Una supernova débil, SN 2005E, desafía los modelos existentes. Su baja masa y su antiguo entorno estelar sugieren un nuevo origen de una enana blanca de acreción de helio, distinta del típico colapso del núcleo o las supernovas de tipo Ia.
Área de la Ciencia:
- La astronomía y la astrofísica.
- Evolución Estelar Evolución Estelar
- Física de las Supernovas Física de las Supernovas
Sus antecedentes:
- Las supernovas tienen su origen en el colapso del núcleo de una estrella masiva (tipo Ib/c, II) o en la detonación de una enana blanca (tipo Ia).
- Las supernovas de tipo Ia ocurren tanto en entornos estelares jóvenes como viejos.
- Las supernovas de colapso de núcleo están vinculadas a poblaciones estelares jóvenes.
Objetivo del estudio:
- Para investigar el origen de SN 2005E, una débil supernova de tipo Ib.
- Para determinar si SN 2005E se ajusta a los modelos establecidos de formación de supernovas.
Principales métodos:
- Análisis de la ubicación de SN 2005E en el antiguo entorno estelar de la galaxia NGC 1032.
- Observaciones espectroscópicas para determinar la composición y la velocidad de la eyección.
- Estimación de la masa del material eyectado.
Principales resultados:
- SN 2005E exhibe una masa expulsada muy baja (~0,3 masas solares).
- La composición de las eyecciones está dominada por productos de combustión de helio, con altas velocidades.
- El entorno de la supernova es una antigua población estelar, inconsistente con el colapso del núcleo.
- La abundancia de calcio es más alta que las supernovas típicas; es probable que esté presente el 44Ti radiactivo.
Conclusiones:
- Las características de SN 2005E argumentan fuertemente en contra de un origen de colapso del núcleo.
- Es poco probable que sea una supernova de tipo Ia subluminosa o regular debido a su composición de eyectos.
- El origen más plausible es un antiguo progenitor de baja masa, probablemente una enana blanca de acreción de helio en un sistema binario.
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