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Signatures of a surviving helium-star companion in type Ia supernovae and constraints on the progenitor companion of SN 2011fe

Single-degenerate (SD) binary systems composed of a white dwarf and a nondegenerate helium (He)-star companion have been proposed as the potential progenitors of Type Ia supernovae (SNe Ia). The He-star companions are expected to survive the SN Ia explosion in this SD progenitor model. In the presen...

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Bibliographic Details
Main Authors: Liu, Zhengwei (Author) , Röpke, Friedrich (Author) , Zeng, Yaotian (Author)
Format: Article (Journal)
Language:English
Published: 2022 April 4
In: The astrophysical journal
Year: 2022, Volume: 928, Issue: 2, Pages: 1-10
ISSN:1538-4357
DOI:10.3847/1538-4357/ac5517
Online Access:Verlag, lizenzpflichtig, Volltext: https://doi.org/10.3847/1538-4357/ac5517
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Author Notes:Zheng-Wei Liu, Friedrich K. Röpke, and Yaotian Zeng
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Summary:Single-degenerate (SD) binary systems composed of a white dwarf and a nondegenerate helium (He)-star companion have been proposed as the potential progenitors of Type Ia supernovae (SNe Ia). The He-star companions are expected to survive the SN Ia explosion in this SD progenitor model. In the present work, we map the surviving He-star companion models computed from our previous three-dimensional hydrodynamical simulations of ejecta-companion interaction into the one-dimensional stellar evolution code Modules for Experiments in Stellar Astrophysics to follow their long-term evolution to make predictions of their post-impact observational properties, which can be helpful in searches for such surviving He-star companions in future observations. By comparing with the very-late-epoch light curve of the best observed SN Ia, SN 2011fe, we find that our surviving He-star companions become significantly more luminous than SN 2011fe about 1000 days after maximum light. This suggests that an He star is very unlikely to be a companion to the progenitor of SN 2011fe.
Item Description:Gesehen am 21.04.2022
Physical Description:Online Resource
ISSN:1538-4357
DOI:10.3847/1538-4357/ac5517

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