Impact of stellar winds on the pair-instability supernova rate
Very massive stars (VMSs, M★ ≥ 100 M⊙) play a crucial role in several astrophysical processes. At low metallicity, they might collapse directly into black holes or end their lives as pair-instability supernovae. Recent observational results set an upper limit of 0.7 yr−1 Gpc−3 on the rate density o...
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| Main Authors: | , , , , , , |
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| Format: | Article (Journal) |
| Language: | English |
| Published: |
November 2025
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| In: |
Astronomy and astrophysics
Year: 2025, Volume: 703, Pages: 1-12 |
| ISSN: | 1432-0746 |
| DOI: | 10.1051/0004-6361/202555490 |
| Online Access: | Verlag, kostenfrei, Volltext: https://doi.org/10.1051/0004-6361/202555490 Verlag, kostenfrei, Volltext: https://www.aanda.org/articles/aa/abs/2025/11/aa55490-25/aa55490-25.html 
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| Author Notes: | Filippo Simonato, Stefano Torniamenti, Michela Mapelli, Giuliano Iorio, Lumen Boco, Franca De Domenico-Langer, and Cecilia Sgalletta |
| Summary: | Very massive stars (VMSs, M★ ≥ 100 M⊙) play a crucial role in several astrophysical processes. At low metallicity, they might collapse directly into black holes or end their lives as pair-instability supernovae. Recent observational results set an upper limit of 0.7 yr−1 Gpc−3 on the rate density of pair-instability supernovae in the nearby Universe. However, most theoretical models predict rates exceeding this limit. In this work, we computed new VMS tracks with the MESA code and used them to analyze the evolution of the (pulsational) pair-instability supernova rate density across cosmic time. We show that stellar-wind models accounting for the transition between optically thin and thick winds yield a pair-instability supernova rate of ℛPISN ~ 0.1 Gpc−3 yr−1 at redshift ɀ ~ 0, which is about two orders of magnitude lower than our previous models. We find that the main contribution to the pair-instability supernova rate comes from stars with metallicities of Z ~ 0.001 − 0.002. Stars with higher metallicities cannot enter the pair-instability supernova regime, even if their zero-age main-sequence mass is up to 500 M⊙. The main reason is that VMSs enter the regime for optically thick winds during the main sequence at metallicities as low as Z ~ 4 × 10−4. This enhances the mass-loss rate, quenching the growth of the He core and thus preventing the onset of pair-instability in later evolutionary stages. This result highlights the critical role of mass loss in shaping the final fate of very massive stars and the rate of pair-instability supernovae. |
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| Item Description: | Online veröffentlicht: 18. November 2025 Gesehen am 03.03.2026 |
| Physical Description: | Online Resource |
| ISSN: | 1432-0746 |
| DOI: | 10.1051/0004-6361/202555490 |