The Type Ic Hypernova SN 2003dh/GRB 030329

By P. Mazzali, J. Deng, Nozomu Tominaga, K. Maeda, K. Nomoto, Thomas Matheson, K. Kawabata, Krzysztof Zbigniew Stanek, P. Garnavich. 2003

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The spectra of SN 2003dh, identified in the afterglow of GRB 030329, are modeled using radiation transport codes. It is shown that SN 2003dh had a high explosion kinetic energy (~4 × 1052 ergs 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 ~0.35 M☉ of 56Ni. 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 km s-1 but more like that of SN 1997ef at lower velocities. The mass of the ejecta is ~8 M☉, somewhat less than in the other two hypernovae. The progenitor must have been a massive star (M ~ 35-40 M☉), as for other hypernovae. The need to combine different one-dimensional explosion models strongly indicates that SN 2003dh was an asymmetric explosion.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Microbiology

View Paper: https://www.semanticscholar.org/paper/7a80f9a9fca71a3811f6c60557d0e9d76cfbb5a4

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Citations in the corpus

The Rates of Hypernovae and Gamma-Ray Bursts: Implications for Their Progenitors (2004, background): “…unambiguous association of a GRB (GRB030329) with a hypernova, SN 2003dh (Hjorth et al. 2003a; Stanek et al. 2003), a highly energetic Type Ic supernova (Mazzali et al. 2003)7, has confirmed that at least some long-duration GRBs are observationally connected with the explosion of massive stars8.”
A POPULATION OF MASSIVE, LUMINOUS GALAXIES HOSTING HEAVILY DUST-OBSCURED GAMMA-RAY BURSTS: IMPLICATIONS FOR THE USE OF GRBs AS TRACERS OF COSMIC STAR FORMATION (2013, background): “…the initial stellar mass function (IMF; van Dokkum & Conroy 2010; Conroy & van Dokkum 2012) could also produce some variation of the GRB rate in relation to other tracers, since GRBs are probably generated only by extremely massive stars (at least 20–50M⊙; Mazzali et al. 2003; Östlin et al. 2008).”
Stellar evolution with rotation - XIII. Predicted GRB rates at various Z (2005, background): “If we consider only WO stars (type Ic supernovae as is the case for SN2003dh/GRB030329, see Mazzali et al. 2003) as GRB progenitors, the GRB production rates are in much better agreement with observations.”
Physical Properties of Wolf-Rayet Stars (2006, background): “Nevertheless, the light curves of broad-lined Type Ic supernovae – SN 1998bw, SN 2003dh and SN 2003lw – suggest ejected core masses of order 10M⊙ (Nakamura et al. 2001; Mazzali et al. 2003; Malesani et al. 2004).”
Supernova Nucleosynthesis in Population III 13-50 M☉ Stars and Abundance Patterns of Extremely Metal-poor Stars (2007, background): “…et al. 1998; Woosley et al. 1999; Nakamura et al. 2001a), GRB 030329/SN 2003dh (Stanek et al. 2003; Hjorth et al. 2003; Matheson et al. 2003; Mazzali et al. 2003; Lipkin et al. 2004; Deng et al. 2005), and GRB 031203/SN 2003lw (Thomsen et al. 2004; Gal-Yam et al. 2004; Cobb et al. 2004;…”
The Supernova Gamma-Ray Burst Connection (2006, background): “Given the broad spectral features, indicating high velocities (∼> 25000 km s −1; Stanek et al. 2003; Hjorth et al. 2003; Mazzali et al. 2003), and apparent absence of hydrogen, helium and strong Si II λ6355 absorption, a classification as Type Ic-BL was natural (Matheson et al., 2003c).”
Mass fall-back and accretion in the central engine of gamma-ray bursts (2008, unknown): “(47) For our canonical model, we estimate the total energy carried away by the wind to be 2 × 1052 erg, which is not dissimilar to the estimated explosion energy in hypernovae associated with GRBs (e.g. Nakamura et al. 2001; Mazzali et al. 2003).”
Early-Time Photometry and Spectroscopy of the Fast Evolving SN 2006aj Associated with GRB 060218 (2006, unknown): “…no hydrogen nor helium in their spectra, but unusually high expansion velocities requiring high explosion energies (Galama et al. 1998; Iwamoto et al. 1998; Patat et al. 2001; Mazzali et al. 2003), in line with the collapsar model for long-duration GRBs (Woosley 1993; MacFadyen & Woosley 1999).”