A new evolution scenario for the over-luminous supernova 2006 gy

Details A new evolution scenario for the over-luminous supernova 2006 gy A new evolution scenario for the over-luminous supernova 2006 gy

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1111..430a&link_type=abstract

PROBING STELLAR POPULATIONS OUT TO THE DISTANT UNIVERSE: CEFALU 2008, Proceedings of the International Conference. AIP Conferen

Computer Science

Supernova Remnants, Stellar Clusters And Associations, Magnitudes And Colors, Luminosities

Scientific paper

We present the photometric and spectroscopic study of the very luminous type IIn SN 2006 gy for a time period spanning more than one year. The evolution of multiband light curves, the pseudo-bolometric (BVRI) light curve and an extended spectral sequence are used to derive constraints on the origin and evolution of the SN. Models of the light curve in the first 170 days suggest that the progenitor was a compact star (R~6-8.1012 cm, Mej~5-14Msolar), and that the SN ejecta collided with massive (6-10Msolar), opaque clumps of previously ejected material. These clumps do not completely obscure the SN photosphere, so that at its peak the luminosity is due both to the decay of 56Ni and to interaction with CSM.

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