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Un destello de rayos X impulsado por una estrella de neutrones asociado con la supernova SN 2006aj
Paolo A Mazzali1, Jinsong Deng, Ken'ichi Nomoto
1Max-Planck Institut für Astrophysik, Karl-Schwarzschild Strasse 1, D-85748 Garching, Germany. mazzali@mpa-garching.mpg.de
Nature
|September 1, 2006
Resumen
Las supernovas vinculadas a las explosiones de rayos gamma (GRB) pueden originarse en estrellas menos masivas de lo que se creía anteriormente. Este hallazgo amplía el rango de masas estelares asociadas con las supernovas GRB y sugiere diversos mecanismos de formación.
Área de la Ciencia:
- La astrofísica es la astrofísica.
- Evolución Estelar Evolución Estelar
- Astronomía de alta energía Astronomía de alta energía
Sus antecedentes:
- Las explosiones de rayos gamma de larga duración (GRB) se asocian típicamente con supernovas hiperenergéticas de estrellas muy masivas (aprox. 40 masas solares).
- La formación de un agujero negro a partir del colapso del progenitor se consideró un requisito previo para el lanzamiento de GRB.
Objetivo del estudio:
- Para investigar las propiedades progenitoras de SN 2006aj, una supernova asociada con un estallido de rayos gamma.
- Para determinar si la conexión supernova-GRB se extiende a un rango más amplio de masas estelares.
Principales métodos:
- Modelado de espectros y curvas de luz de la supernova SN 2006aj.
- Comparación de las propiedades de SN 2006aj con otras supernovas asociadas al GRB.
Principales resultados:
- SN 2006aj exhibió una energía de explosión y masa expulsada significativamente más bajas en comparación con otras supernovas GRB.
- Estas propiedades sugieren una estrella progenitora con una masa inicial de aproximadamente 20 masas solares, probablemente formando una estrella de neutrones.
- El más débil GRB 060218 (Rayo X flash) y el flujo de radio de SN 2006aj se alinean con este evento de menor energía.
Conclusiones:
- La conexión supernova-GRB abarca un rango más amplio de masas estelares de lo que se suponía anteriormente.
- Estrellas menos masivas (aprox. 20 masas solares) pueden producir GRB a través de mecanismos que involucran la actividad magnética de estrellas de neutrones nacientes, distintas del modelo de colapso para estrellas más masivas.
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