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Date and Time of the Query: 2019-08-19 T20:28:21 PDT
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For refcode 2012A&A...546A..28J:
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Copyright by European Southern Observatory (ESO). Reproduced by permission
2012A&A...546A..28J The progenitor mass of the Type IIP supernova SN 2004et from late-time spectral modeling Jerkstrand, A.; Fransson, C.; Maguire, K.; Smartt, S.; Ergon, M.; Spyromilio, J. Abstract. 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 M_ZAMS_ = 15 M_sun_ progenitor star (with an oxygen mass of 0.8 M_sun_) to satisfactorily reproduce [O i] lambdalambda6300, 6364 and other emission lines of carbon, sodium, magnesium, and silicon, while 12 M_sun_ and 19 M_sun_ 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 {rho}(t) ~= 7 x 10^-14^ x (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. Appendices are available in electronic form at http://www.aanda.org Key words: supernovae: general, supernovae: individual: SN 2004et, line: formation, line: identification, radiative transfer
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