Long-term Evolution of Postexplosion Helium-star Companions of Type Iax Supernovae

Yaotian Zeng; Zheng Wei Liu; Alexander Heger; Curtis McCully; Friedrich K. Röpke; Zhanwen Han

doi:10.3847/1538-4357/ac75bb

Long-term Evolution of Postexplosion Helium-star Companions of Type Iax Supernovae

Yaotian Zeng, Zheng Wei Liu, Alexander Heger, Curtis McCully, Friedrich K. Röpke, Zhanwen Han

School of Physics and Astronomy

Research output: Contribution to journal › Article › Research › peer-review

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Abstract

Supernovae of Type Iax (SNe Iax) are an accepted faint subclass of hydrogen-free supernovae. Their origin, the nature of the progenitor systems, however, is an open question. Recent studies suggest that the weak deflagration explosion of a near-Chandrasekhar-mass white dwarf in a binary system with a helium-star donor could be the origin of SNe Iax. In this scenario, the helium-star donor is expected to survive the explosion. We use the one-dimensional stellar evolution codes MESA and Kepler to follow the postimpact evolution of the surviving helium companion stars. The stellar models are based on our previous hydrodynamical simulations of ejecta-donor interaction, and we explore the observational characteristics of these surviving helium companions. We find that the luminosities of the surviving helium companions increase significantly after the impact: they could vary from 2500 L ⊙ to 16,000 L ⊙ for a Kelvin-Helmholtz timescale of about 104 yr. After the star reaches thermal equilibrium, it evolves as an O-type hot subdwarf (sdO) star and continues its evolution along the evolutionary track of a normal sdO star with the same mass. Our results will help to identify the surviving helium companions of SNe Iax in future observations and to place new constraints on their progenitor models.

Original language	English
Article number	65
Number of pages	10
Journal	The Astrophysical Journal
Volume	933
Issue number	1
DOIs	https://doi.org/10.3847/1538-4357/ac75bb
Publication status	Published - 1 Jul 2022

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10.3847/1538-4357/ac75bbLicence: CC BY

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title = "Long-term Evolution of Postexplosion Helium-star Companions of Type Iax Supernovae",

abstract = "Supernovae of Type Iax (SNe Iax) are an accepted faint subclass of hydrogen-free supernovae. Their origin, the nature of the progenitor systems, however, is an open question. Recent studies suggest that the weak deflagration explosion of a near-Chandrasekhar-mass white dwarf in a binary system with a helium-star donor could be the origin of SNe Iax. In this scenario, the helium-star donor is expected to survive the explosion. We use the one-dimensional stellar evolution codes MESA and Kepler to follow the postimpact evolution of the surviving helium companion stars. The stellar models are based on our previous hydrodynamical simulations of ejecta-donor interaction, and we explore the observational characteristics of these surviving helium companions. We find that the luminosities of the surviving helium companions increase significantly after the impact: they could vary from 2500 L ⊙ to 16,000 L ⊙ for a Kelvin-Helmholtz timescale of about 104 yr. After the star reaches thermal equilibrium, it evolves as an O-type hot subdwarf (sdO) star and continues its evolution along the evolutionary track of a normal sdO star with the same mass. Our results will help to identify the surviving helium companions of SNe Iax in future observations and to place new constraints on their progenitor models. ",

author = "Yaotian Zeng and Liu, {Zheng Wei} and Alexander Heger and Curtis McCully and R{\"o}pke, {Friedrich K.} and Zhanwen Han",

note = "Funding Information: We thank the anonymous referee for his/her helpful comments. We thank Xiangcun Meng, Hailiang Chen, and Jiajia Li for their useful discussions. Y.T.Z. would like to thank Yangyang Zhang and Heran Xiong for their helping of using the MESA . This work is supported by the National Key R&D Program of China (Nos. 2021YFA1600401 and 2021YFA1600400), the National Natural Science Foundation of China (NSFC, Nos. 11873016 and 11733008), the Chinese Academy of Sciences, and Yunnan Province (Nos. 12090040, 12090043, 202001AW070007, 2019HA012, and 2017HC018). A.H. was supported, in part, by the Australian Research Council (ARC) Centre of Excellence (CoE) for Gravitational Wave Discovery (OzGrav) through project number CE170100004, by the ARC CoE for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) through project number CE170100013, and by the National Science Foundation under grant No. PHY-1430152 (JINA Center for the Evolution of the Elements, JINA-CEE). The work of F.K.R. is supported by the Klaus Tschira Foundation and by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation)—Project-ID 138713538—SFB 881 (“The Milky Way System”, Subproject A10). The authors gratefully acknowledge the “PHOENIX Supercomputing Platform” jointly operated by the Binary Population Synthesis Group and the Stellar Astrophysics Group at Yunnan Observatories, Chinese Academy of Sciences. This work made use of the Heidelberg Supernova Model Archive (HESMA, Kromer et al. , see https://hesma.h-its.org ). Publisher Copyright: {\textcopyright} 2022. The Author(s). Published by the American Astronomical Society.",

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doi = "10.3847/1538-4357/ac75bb",

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AU - Zeng, Yaotian

AU - Liu, Zheng Wei

AU - Heger, Alexander

AU - McCully, Curtis

AU - Röpke, Friedrich K.

AU - Han, Zhanwen

N1 - Funding Information: We thank the anonymous referee for his/her helpful comments. We thank Xiangcun Meng, Hailiang Chen, and Jiajia Li for their useful discussions. Y.T.Z. would like to thank Yangyang Zhang and Heran Xiong for their helping of using the MESA . This work is supported by the National Key R&D Program of China (Nos. 2021YFA1600401 and 2021YFA1600400), the National Natural Science Foundation of China (NSFC, Nos. 11873016 and 11733008), the Chinese Academy of Sciences, and Yunnan Province (Nos. 12090040, 12090043, 202001AW070007, 2019HA012, and 2017HC018). A.H. was supported, in part, by the Australian Research Council (ARC) Centre of Excellence (CoE) for Gravitational Wave Discovery (OzGrav) through project number CE170100004, by the ARC CoE for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) through project number CE170100013, and by the National Science Foundation under grant No. PHY-1430152 (JINA Center for the Evolution of the Elements, JINA-CEE). The work of F.K.R. is supported by the Klaus Tschira Foundation and by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation)—Project-ID 138713538—SFB 881 (“The Milky Way System”, Subproject A10). The authors gratefully acknowledge the “PHOENIX Supercomputing Platform” jointly operated by the Binary Population Synthesis Group and the Stellar Astrophysics Group at Yunnan Observatories, Chinese Academy of Sciences. This work made use of the Heidelberg Supernova Model Archive (HESMA, Kromer et al. , see https://hesma.h-its.org ). Publisher Copyright: © 2022. The Author(s). Published by the American Astronomical Society.

PY - 2022/7/1

Y1 - 2022/7/1

N2 - Supernovae of Type Iax (SNe Iax) are an accepted faint subclass of hydrogen-free supernovae. Their origin, the nature of the progenitor systems, however, is an open question. Recent studies suggest that the weak deflagration explosion of a near-Chandrasekhar-mass white dwarf in a binary system with a helium-star donor could be the origin of SNe Iax. In this scenario, the helium-star donor is expected to survive the explosion. We use the one-dimensional stellar evolution codes MESA and Kepler to follow the postimpact evolution of the surviving helium companion stars. The stellar models are based on our previous hydrodynamical simulations of ejecta-donor interaction, and we explore the observational characteristics of these surviving helium companions. We find that the luminosities of the surviving helium companions increase significantly after the impact: they could vary from 2500 L ⊙ to 16,000 L ⊙ for a Kelvin-Helmholtz timescale of about 104 yr. After the star reaches thermal equilibrium, it evolves as an O-type hot subdwarf (sdO) star and continues its evolution along the evolutionary track of a normal sdO star with the same mass. Our results will help to identify the surviving helium companions of SNe Iax in future observations and to place new constraints on their progenitor models.

AB - Supernovae of Type Iax (SNe Iax) are an accepted faint subclass of hydrogen-free supernovae. Their origin, the nature of the progenitor systems, however, is an open question. Recent studies suggest that the weak deflagration explosion of a near-Chandrasekhar-mass white dwarf in a binary system with a helium-star donor could be the origin of SNe Iax. In this scenario, the helium-star donor is expected to survive the explosion. We use the one-dimensional stellar evolution codes MESA and Kepler to follow the postimpact evolution of the surviving helium companion stars. The stellar models are based on our previous hydrodynamical simulations of ejecta-donor interaction, and we explore the observational characteristics of these surviving helium companions. We find that the luminosities of the surviving helium companions increase significantly after the impact: they could vary from 2500 L ⊙ to 16,000 L ⊙ for a Kelvin-Helmholtz timescale of about 104 yr. After the star reaches thermal equilibrium, it evolves as an O-type hot subdwarf (sdO) star and continues its evolution along the evolutionary track of a normal sdO star with the same mass. Our results will help to identify the surviving helium companions of SNe Iax in future observations and to place new constraints on their progenitor models.

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JO - The Astrophysical Journal

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Long-term Evolution of Postexplosion Helium-star Companions of Type Iax Supernovae

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ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions

ARC Centre of Excellence for Gravitational Wave Discovery

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Long-term Evolution of Postexplosion Helium-star Companions of Type Iax Supernovae

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ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions

ARC Centre of Excellence for Gravitational Wave Discovery

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