Volume 546, October 2012
|Number of page(s)||21|
|Section||Stellar structure and evolution|
|Published online||01 October 2012|
The progenitor mass of the Type IIP supernova SN 2004et from late-time spectral modeling⋆
Department of Astronomy, The Oskar Klein CentreStockholm
2 Astrophysics Research Centre, School of Maths and Physics, Queen’s University Belfast, Belfast BT7 1NN, UK
3 Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH, UK
4 ESO, Karl-Schwarzschild-Strasse 2, 85748 Garching, Germany
Received: 3 May 2012
Accepted: 8 August 2012
SN 2004et is one of the nearest and best-observed Type IIP supernovae, with a progenitor detection as well as good photometric and spectroscopic observational coverage well into the nebular phase. Based on nucleosynthesis from stellar evolution/explosion models we apply spectral modeling to analyze its 140−700 day evolution from ultraviolet to mid-infrared. We find a MZAMS = 15 M⊙ progenitor star (with an oxygen mass of 0.8 M⊙) to satisfactorily reproduce [O i] λλ6300, 6364 and other emission lines of carbon, sodium, magnesium, and silicon, while 12 M⊙ and 19 M⊙ models under- and overproduce most of these lines, respectively. This result is in fair agreement with the mass derived from the progenitor detection, but in disagreement with hydrodynamical modeling of the early-time light curve. From modeling of the mid-infrared iron-group emission lines, we determine the density of the “Ni-bubble” to ρ(t) ≃ 7 × 10-14 × (t/100 d)-3 g cm-3, corresponding to a filling factor of f = 0.15 in the metal core region (V = 1800 km s-1). We also confirm that silicate dust, CO, and SiO emission are all present in the spectra.
Key words: supernovae: general / supernovae: individual: SN 2004et / line: formation / line: identification / radiative transfer
Appendices are available in electronic form at http://www.aanda.org
© ESO, 2012
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