Abundance stratification in Type Ia Supernovae - IV: the luminous, peculiar SN 1991T

TL;DR

This study models the element distribution in the ejecta of the peculiar, luminous Type Ia supernova SN 1991T using spectral data over time, revealing its unique stratification and supporting the delayed detonation explosion model.

Contribution

It provides detailed abundance stratification of SN 1991T and compares W7 and WDD3 models, favoring WDD3 for better spectral fits and insights into explosion mechanisms.

Findings

WDD3 model fits spectra better than W7

Core dominated by stable Fe and 56Ni distribution

Outer layers mainly oxygen with minimal carbon detection

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 model 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 solar masses, as in most SNe Ia. The layer above is mainly 56Ni up to v~10000 km/s (~0.78 solar masses). A significant amount of 56Ni (~3 %) is located in the outer layers. A narrow layer between 10000 km/s and ~12000 km/s is dominated by intermediate mass elements (IME), ~0.18 solar masses. 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 solar masses. Carbon lines are never detected, yielding an upper limit of 0.01 solar masses 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.