A very luminous magnetar-powered supernova associated with an ultra-long [gamma]-ray burst
- Autores: Jochen Greiner, P. A. Mazzali, Alexander D. Kann, Thomas Krühler, Elena Pian, Simon Prentice
- Localización: Nature: International weekly journal of science, ISSN 0028-0836, Vol. 523, Nº 7559, 2015, págs. 189-192
- Idioma: inglés
- DOI: 10.1038/nature14579
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Resumen
A new class of ultra-long-duration (more than 10,000 seconds) [gamma]-ray bursts has recently been suggested1,2,3. They may originate in the explosion of stars with much larger radii than those producing normal long-duration [gamma]-ray bursts3,4 or in the tidal disruption of a star3. No clear supernova has yet been associated with an ultra-long-duration [gamma]-ray burst. Here we report that a supernova (SN 2011kl) was associated with the ultra-long-duration [gamma]-ray burst GRB 111209A, at a redshift z of 0.677. This supernova is more than three times more luminous than type Ic supernovae associated with long-duration [gamma]-ray bursts5,6,7, and its spectrum is distinctly different. The slope of the continuum resembles those of super-luminous supernovae8,9, but extends further down into the rest-frame ultraviolet implying a low metal content. The light curve evolves much more rapidly than those of super-luminous supernovae. This combination of high luminosity and low metal-line opacity cannot be reconciled with typical type Ic supernovae, but can be reproduced by a model where extra energy is injected by a strongly magnetized neutron star (a magnetar), which has also been proposed as the explanation for super-luminous supernovae10.
