Three-dimensional simulations of gravitationally confined detonations compared to observations of SN 1991T

TL;DR

This study uses 3D simulations to explore the gravitationally confined detonation model for Type Ia supernovae, comparing synthetic observables with actual supernova data, and finds notable discrepancies with SN 1991T.

Contribution

The paper presents a detailed 3D simulation of the GCD model, including nucleosynthesis and synthetic observables, and compares these with observations of SN 1991T to evaluate the model's validity.

Findings

Synthetic light curves show viewing-angle sensitivity inconsistent with observations.

Model predicts spectral features that are too strong compared to SN 1991T.

Chemical abundance stratification in the model does not match observed supernova data.

Abstract

The gravitationally confined detonation (GCD) model has been proposed as a possible explosion mechanism for Type Ia supernovae in the single-degenerate evolution channel. Driven by buoyancy, a deflagration flame rises in a narrow cone towards the surface. For the most part, the flow of the expanding ashes remains radial, but upon reaching the outer, low-pressure layers of the white dwarf, an additional lateral component develops. This makes the deflagration ashes converge again at the opposite side, where the compression heats fuel and a detonation may be launched. To test the GCD explosion model, we perform a 3D simulation for a model with an ignition spot offset near the upper limit of what is still justifiable, 200 km. This simulation meets our deliberately optimistic detonation criteria and we initiate a detonation. The detonation burns through the white dwarf and leads to its complete disruption. We determine nucleosynthetic yields by post-processing 10^6 tracer particles with a 384 nuclide reaction network and we present multi-band light curves and time-dependent optical spectra. We find that our synthetic observables show a prominent viewing-angle sensitivity in UV and blue bands, which is in tension with observed SNe Ia. The strong dependence on viewing-angle is caused by the asymmetric distribution of the deflagration ashes in the outer ejecta layers. Finally, we perform a comparison of our model to SN 1991T. The overall flux-level of the model is slightly too low and the model predicts pre-maximum light spectral features due to Ca, S, and Si that are too strong. Furthermore, the model chemical abundance stratification qualitatively disagrees with recent abundance tomography results in two key areas: our model lacks low velocity stable Fe and instead has copious amounts of high-velocity 56Ni and stable Fe. We therefore do not find good agreement of the model with SN 1991T.