4.7 Article

3D deflagration simulations leaving bound remnants: a model for 2002cx-like Type Ia supernovae

Journal

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 429, Issue 3, Pages 2287-2297

Publisher

OXFORD UNIV PRESS
DOI: 10.1093/mnras/sts498

Keywords

hydrodynamics; radiative transfer; methods: numerical; techniques: spectroscopic; supernovae: individual: SN 2005hk

Funding

  1. European Union [HPRN-CT-2002-00303]
  2. Deutsche Forschungsgemeinschaft via the Transregional Collaborative Research Center TRR 33 'The Dark Universe'
  3. Excellence Cluster EXC153 'Origin and Structure of the Universe'
  4. Emmy Noether Programme [RO 3676/1-1]
  5. Group of Eight/Deutscher Akademischer Austausch Dienst (Go8/DAAD) exchange programme
  6. [076.D-0183]
  7. [GTC19-12A]

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2002cx-like supernovae are a sub-class of sub-luminous Type Ia supernovae (SNe). Their light curves and spectra are characterized by distinct features that indicate strong mixing of the explosion ejecta. Pure turbulent deflagrations have been shown to produce such mixed ejecta. Here, we present hydrodynamics, nucleosynthesis and radiative-transfer calculations for a 3D full-star deflagration of a Chandrasekhar-mass white dwarf. Our model is able to reproduce the characteristic observational features of SN 2005hk (a prototypical 2002cx-like supernova), not only in the optical, but also in the near-infrared. For that purpose we present, for the first time, five near-infrared spectra of SN 2005hk from -0.2 to 26.6 d with respect to B-band maximum. Since our model burns only small parts of the initial white dwarf, it fails to completely unbind the white dwarf and leaves behind a bound remnant of similar to 1.03 M-circle dot - consisting mainly of unburned carbon and oxygen, but also enriched by some amount of intermediate-mass and iron-group elements from the explosion products that fall back on the remnant. We discuss possibilities for detecting this bound remnant and how it might influence the late-time observables of 2002cx-like SNe.

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