Please use this identifier to cite or link to this item: https://hdl.handle.net/2440/116914
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Type: Journal article
Title: Abundance stratification in type Ia supernovae - IV. The luminous, peculiar SN 1991T
Author: Sasdelli, M.
Mazzali, P.
Pian, E.
Nomoto, K.
Hachinger, S.
Cappellaro, E.
Benetti, S.
Citation: Monthly Notices of the Royal Astronomical Society, 2014; 445(1):711-725
Publisher: Oxford University Press
Issue Date: 2014
ISSN: 0035-8711
1365-2966
Statement of
Responsibility: 
Michele Sasdelli, P. A. Mazzali, E. Pian, K. Nomoto, S. Hachinger, E. Cappellaro and S. Benetti
Abstract: The abundance distribution of the elements in the ejecta of the peculiar, luminous Type Ia supernova (SN Ia) 1991T is obtained modelling spectra from before maximum light until a year after the explosion, with the method of ‘Abundance Tomography’. SN 1991T is different from other slowly declining SNe Ia (e.g. SN 1999ee) in having a weaker Si ii 6355 line and strong features of iron group elements before maximum. The distance to the SN is investigated along with the abundances and the density profile. The ionization transition that happens around maximum sets a strict upper limit on the luminosity. Both W7 and the WDD3 delayed detonation models are tested. WDD3 is found to provide marginally better fits. In this model the core of the ejecta is dominated by stable Fe with a mass of about 0.15 M⊙, as in most SNe Ia. The layer above is mainly 56Ni up to v ∼ 10 000 km s−1 (≈0.78 M⊙). A significant amount of 56Ni (∼3 per cent) is located in the outer layers. A narrow layer between 10 000 km s−1 and ∼12 000 km s−1 is dominated by intermediate-mass elements (IME), ∼0.18 M⊙. This is small for a SN Ia. The high luminosity and the consequently high ionization, and the high 56Ni abundance at high velocities, explain the peculiar early-time spectra of SN 1991T. The outer part is mainly of oxygen, ∼0.3 M⊙. Carbon lines are never detected, yielding an upper limit of 0.01 M⊙ for C. The abundances obtained with the W7 density model are qualitatively similar to those of the WDD3 model. Different elements are stratified with moderate mixing, resembling a delayed detonation.
Rights: 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
DOI: 10.1093/mnras/stu1777
Published version: http://dx.doi.org/10.1093/mnras/stu1777
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