Physics-driven Explosions of Stripped High-mass Stars: Synthetic Light Curves and Spectra of Stripped-envelope Supernovae with Broad Light Curves
Stripped-envelope supernovae (SESNe) represent a significant fraction of core-collapse supernovae, arising from massive stars that have shed their hydrogen and, in some cases, helium envelopes. The origins and explosion mechanisms of SESNe remain a topic of active investigation. In this work, we emp...
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2025-01-01
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| author | Jing Lu Brandon L. Barker Jared Goldberg Wolfgang E. Kerzendorf Maryam Modjaz Sean M. Couch Joshua V. Shields Andrew G. Fullard |
| author_facet | Jing Lu Brandon L. Barker Jared Goldberg Wolfgang E. Kerzendorf Maryam Modjaz Sean M. Couch Joshua V. Shields Andrew G. Fullard |
| author_sort | Jing Lu |
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| description | Stripped-envelope supernovae (SESNe) represent a significant fraction of core-collapse supernovae, arising from massive stars that have shed their hydrogen and, in some cases, helium envelopes. The origins and explosion mechanisms of SESNe remain a topic of active investigation. In this work, we employ radiative-transfer simulations to model the light curves and spectra of a set of explosions of single, solar-metallicity, massive Wolf–Rayet stars with ejecta masses ranging from 4 to 11 M _⊙ , which were computed from a turbulence-aided and neutrino-driven explosion mechanism. We analyze these synthetic observables to explore the impact of varying ejecta mass and helium content on observable features. We find that the light curve shape of these progenitors with high ejecta masses is consistent with observed SESNe with broad light curves but not the peak luminosities. The commonly used analytic formula based on rising bolometric light curves overestimates the ejecta mass of these high-initial-mass progenitor explosions by a factor of up to 2.6. In contrast, the calibrated method by Haynie et al., which relies on late-time decay tails, reduces uncertainties to an average of 20% within the calibrated ejecta mass range. Spectroscopically, the He i 1.083 μ m line remains prominent even in models with as little as 0.02 M _⊙ of helium. However, the strength of the optical He i lines is not directly proportional to the helium mass but instead depends on a complex interplay of factors such as the ^56 Ni distribution, composition, and radiation field. Thus, producing realistic helium features requires detailed radiative transfer simulations for each new hydrodynamic model. |
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| publishDate | 2025-01-01 |
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| spelling | doaj-art-8cdec95649b6452fbf7d5206acd8c6632025-01-23T07:53:46ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01979214810.3847/1538-4357/ada26dPhysics-driven Explosions of Stripped High-mass Stars: Synthetic Light Curves and Spectra of Stripped-envelope Supernovae with Broad Light CurvesJing Lu0https://orcid.org/0000-0002-3900-1452Brandon L. Barker1https://orcid.org/0000-0002-8825-0893Jared Goldberg2https://orcid.org/0000-0003-1012-3031Wolfgang E. Kerzendorf3https://orcid.org/0000-0002-0479-7235Maryam Modjaz4https://orcid.org/0000-0001-7132-0333Sean M. Couch5https://orcid.org/0000-0002-5080-5996Joshua V. Shields6https://orcid.org/0000-0002-1560-5286Andrew G. Fullard7https://orcid.org/0000-0001-7343-1678Department of Physics and Astronomy, Michigan State University , East Lansing, MI 48824, USA ; lujing8@msu.eduComputational Physics and Methods , Los Alamos National Laboratory, Los Alamos, NM 87545, USA; Center for Theoretical Astrophysics , Los Alamos National Laboratory, Los Alamos, NM 87545, USACenter for Computational Astrophysics, Flatiron Institute , 162 5th Avenue, New York, NY 10010, USADepartment of Physics and Astronomy, Michigan State University , East Lansing, MI 48824, USA ; lujing8@msu.edu; Department of Computational Mathematics, Science, and Engineering, Michigan State University , East Lansing, MI 48824, USADepartment of Astronomy, University of Virginia , Charlottesville, VA 22904, USADepartment of Physics and Astronomy, Michigan State University , East Lansing, MI 48824, USA ; lujing8@msu.edu; Department of Computational Mathematics, Science, and Engineering, Michigan State University , East Lansing, MI 48824, USA; Joint Institute for Nuclear Astrophysics-Center for the Evolution of the Elements, Michigan State University , East Lansing, MI 48824, USA; National Superconducting Cyclotron Laboratory, Michigan State University , East Lansing, MI 48824, USADepartment of Physics and Astronomy, Michigan State University , East Lansing, MI 48824, USA ; lujing8@msu.eduDepartment of Physics and Astronomy, Michigan State University , East Lansing, MI 48824, USA ; lujing8@msu.eduStripped-envelope supernovae (SESNe) represent a significant fraction of core-collapse supernovae, arising from massive stars that have shed their hydrogen and, in some cases, helium envelopes. The origins and explosion mechanisms of SESNe remain a topic of active investigation. In this work, we employ radiative-transfer simulations to model the light curves and spectra of a set of explosions of single, solar-metallicity, massive Wolf–Rayet stars with ejecta masses ranging from 4 to 11 M _⊙ , which were computed from a turbulence-aided and neutrino-driven explosion mechanism. We analyze these synthetic observables to explore the impact of varying ejecta mass and helium content on observable features. We find that the light curve shape of these progenitors with high ejecta masses is consistent with observed SESNe with broad light curves but not the peak luminosities. The commonly used analytic formula based on rising bolometric light curves overestimates the ejecta mass of these high-initial-mass progenitor explosions by a factor of up to 2.6. In contrast, the calibrated method by Haynie et al., which relies on late-time decay tails, reduces uncertainties to an average of 20% within the calibrated ejecta mass range. Spectroscopically, the He i 1.083 μ m line remains prominent even in models with as little as 0.02 M _⊙ of helium. However, the strength of the optical He i lines is not directly proportional to the helium mass but instead depends on a complex interplay of factors such as the ^56 Ni distribution, composition, and radiation field. Thus, producing realistic helium features requires detailed radiative transfer simulations for each new hydrodynamic model.https://doi.org/10.3847/1538-4357/ada26dCore-collapse supernovaeRadiative transfer simulationsSupernovaeComputational methodsSupernova dynamics |
| spellingShingle | Jing Lu Brandon L. Barker Jared Goldberg Wolfgang E. Kerzendorf Maryam Modjaz Sean M. Couch Joshua V. Shields Andrew G. Fullard Physics-driven Explosions of Stripped High-mass Stars: Synthetic Light Curves and Spectra of Stripped-envelope Supernovae with Broad Light Curves The Astrophysical Journal Core-collapse supernovae Radiative transfer simulations Supernovae Computational methods Supernova dynamics |
| title | Physics-driven Explosions of Stripped High-mass Stars: Synthetic Light Curves and Spectra of Stripped-envelope Supernovae with Broad Light Curves |
| title_full | Physics-driven Explosions of Stripped High-mass Stars: Synthetic Light Curves and Spectra of Stripped-envelope Supernovae with Broad Light Curves |
| title_fullStr | Physics-driven Explosions of Stripped High-mass Stars: Synthetic Light Curves and Spectra of Stripped-envelope Supernovae with Broad Light Curves |
| title_full_unstemmed | Physics-driven Explosions of Stripped High-mass Stars: Synthetic Light Curves and Spectra of Stripped-envelope Supernovae with Broad Light Curves |
| title_short | Physics-driven Explosions of Stripped High-mass Stars: Synthetic Light Curves and Spectra of Stripped-envelope Supernovae with Broad Light Curves |
| title_sort | physics driven explosions of stripped high mass stars synthetic light curves and spectra of stripped envelope supernovae with broad light curves |
| topic | Core-collapse supernovae Radiative transfer simulations Supernovae Computational methods Supernova dynamics |
| url | https://doi.org/10.3847/1538-4357/ada26d |
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