Models of pulsationally assisted gravitationally confined detonations with different ignition conditions

F. Lach, F. P. Callan, S. A. Sim, F. K. Röpke

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9 Citations (Scopus)

Abstract

Over the past decades, many explosion scenarios for Type Ia supernovae have been proposed and investigated including various combinations of deflagrations and detonations in white dwarfs of different masses up to the Chandrasekhar mass. One of these is the gravitationally confined detonation model. In this case a weak deflagration burns to the surface, wraps around the bound core, and collides at the antipode. A subsequent detonation is then initiated in the collision area. Since the parameter space for this scenario, that is, varying central densities and ignition geometries, has not been studied in detail, we used pure deflagration models of a previous parameter study dedicated to Type Iax supernovae as initial models to investigate the gravitationally confined detonation scenario. We aim to judge whether this channel can account for one of the many subgroups of Type Ia supernovae, or even normal events. To this end, we employed a comprehensive pipeline for three-dimensional Type Ia supernova modeling that consists of hydrodynamic explosion simulations, nuclear network calculations, and radiative transfer. The observables extracted from the radiative transfer are then compared to observed light curves and spectra. The study produces a wide range in masses of synthesized 56Ni ranging from 0.257 to 1.057 M⊙, and, thus, can potentially account for subluminous as well as overluminous Type Ia supernovae in terms of brightness. However, a rough agreement with observed light curves and spectra can only be found for 91T-like objects. Although several discrepancies remain, we conclude that the gravitationally confined detonation model cannot be ruled out as a mechanism to produce 91T-like objects. However, the models do not provide a good explanation for either normal Type Ia supernovae or Type Iax supernovae.

Original languageEnglish
Article numberA27
Number of pages15
JournalAstronomy and Astrophysics
Volume659
DOIs
Publication statusPublished - 02 Mar 2022

Bibliographical note

Funding Information:
Acknowledgements. This work was supported by the Deutsche Forschungsge-meinschaft (DFG, German Research Foundation) – Project-ID 138713538 – SFB 881 (“The Milky Way System”, subproject A10), by the ChETEC COST Action (CA16117), and by the National Science Foundation under Grant No. OISE-1927130 (IReNA). FL and FKR acknowledge support by the Klaus Tschira Foundation. FPC acknowledges an STFC studentship and SAS acknowledges funding from STFC Grant Ref: ST/P000312/1. NumPy and SciPy (Oliphant 2007), IPython (Pérez & Granger 2007), and Matplotlib (Hunter 2007) were used for data processing and plotting. The authors gratefully acknowledge the Gauss Centre for Supercomputing e.V. (www.gauss-centre.eu) for funding this project by providing computing time on the GCS Supercomputer JUWELS (Jülich Supercomputing Centre 2019) at Jülich Supercomputing Centre (JSC). Part of this work was performed using the Cambridge Service for Data Driven Discovery (CSD3), part of which is operated by the University of Cambridge Research Computing on behalf of the STFC DiRAC HPC Facility (www.dirac. ac.uk). The DiRAC component of CSD3 was funded by BEIS capital funding via STFC capital grants ST/P002307/1 and ST/R002452/1 and STFC operations grant ST/R00689X/1. DiRAC is part of the National e-Infrastructure. We thank James Gillanders for assisting with the flux calibrations of the observed spectra.

Publisher Copyright:
© 2022 ESO.

Keywords

  • Hydrodynamics
  • Methods: Numerical
  • Nuclear reactions, nucleosynthesis, abundances
  • Radiative transfer
  • Supernovae: General
  • Supernovae: Individual: SN 1991T

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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