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The Type Ic Hypernova SN 2003dh/GRB 030329

Paolo A. MazzaliDepartment of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, JapanJinsong DengDepartment of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, JapanNozomu TominagaDepartment of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, JapanKeiichi MaedaDepartment of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, JapanKen'ichi NomotoDepartment of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, JapanThomas MathesonHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138Koji S. KawabataOptical and Infrared Astronomy Division, NAOJ, Mitaka, Tokyo 181-8588, JapanKrzysztof Z. StanekHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138Peter M. GarnavichDepartment of Physics, University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, IN 46556

2003en

ABI

Annotatsiya

The spectra of SN 2003dh, identified in the afterglow of GRB030329, are modeled using radiation transport codes. It is shown that SN 2003dh had a high explosion kinetic energy ($\sim 4 \times 10^{52}$ erg in spherical symmetry), making it one of the most powerful hypernovae observed so far, and supporting the case for association between hypernovae and Gamma Ray Bursts. However, the light curve derived from fitting the spectra suggests that SN 2003dh was not as bright as SN 1998bw, ejecting only $\sim 0.35\Msun$ of \Nifs. The spectra of SN 2003dh resemble those of SN 1998bw around maximum, but later they look more like those of the less energetic hypernova SN 1997ef. The spectra and the inferred light curve can be modeled adopting a density distribution similar to that used for SN 1998bw at $ v > 25,000$\kms but more like that of SN 1997ef at lower velocities. The mass of the ejecta is $\sim 8\Msun$, somewhat less than in the other two hypernovae. The progenitor must have been a massive star ($M \sim 35-40\Msun$), as for other hypernovae. The need to combine different one-dimensional explosion models strongly indicates that SN 2003dh was an asymmetric explosion.

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DOI: 10.1086/381259

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