A Model for Eruptive Mass Loss in Massive Stars
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arXiv
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| Autores principales: | , , , , , |
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| Formato: | Preprint |
| Publicado: |
2024
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| _version_ | 1866914940853420032 |
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| author | Cheng, Shelley J. Goldberg, Jared A. Cantiello, Matteo Bauer, Evan B. Renzo, Mathieu Conroy, Charlie |
| author_facet | Cheng, Shelley J. Goldberg, Jared A. Cantiello, Matteo Bauer, Evan B. Renzo, Mathieu Conroy, Charlie |
| contents | Eruptive mass loss in massive stars is known to occur, but the mechanism(s) are not yet well-understood. One proposed physical explanation appeals to opacity-driven super-Eddington luminosities in stellar envelopes. Here, we present a 1D model for eruptive mass loss and implement this model in the MESA stellar evolution code. The model identifies regions in the star where the energy associated with a locally super-Eddington luminosity exceeds the binding energy of the overlaying envelope. The material above such regions is ejected from the star. Stars with masses $10-100~M_\odot$ at solar and SMC metallicities are evolved through core helium burning, with and without this new eruptive mass-loss scheme. We find that eruptive mass loss of up to $\sim10^{-2}~M_\odot \mathrm{yr}^{-1}$ can be driven by this mechanism, and occurs in a vertical band on the HR diagram between $3.5 \lesssim \log(T_\mathrm{eff}/\mathrm{K}) \lesssim 4.0$. This predicted eruptive mass loss prevents stars of initial masses $\gtrsim20~M_\odot$ from evolving to become red supergiants, with the stars instead ending their lives as blue supergiants, and therefore offers a possible explanation for the observed lack of red supergiants in that mass regime. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2405_12274 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | A Model for Eruptive Mass Loss in Massive Stars Cheng, Shelley J. Goldberg, Jared A. Cantiello, Matteo Bauer, Evan B. Renzo, Mathieu Conroy, Charlie Solar and Stellar Astrophysics Astrophysics of Galaxies Eruptive mass loss in massive stars is known to occur, but the mechanism(s) are not yet well-understood. One proposed physical explanation appeals to opacity-driven super-Eddington luminosities in stellar envelopes. Here, we present a 1D model for eruptive mass loss and implement this model in the MESA stellar evolution code. The model identifies regions in the star where the energy associated with a locally super-Eddington luminosity exceeds the binding energy of the overlaying envelope. The material above such regions is ejected from the star. Stars with masses $10-100~M_\odot$ at solar and SMC metallicities are evolved through core helium burning, with and without this new eruptive mass-loss scheme. We find that eruptive mass loss of up to $\sim10^{-2}~M_\odot \mathrm{yr}^{-1}$ can be driven by this mechanism, and occurs in a vertical band on the HR diagram between $3.5 \lesssim \log(T_\mathrm{eff}/\mathrm{K}) \lesssim 4.0$. This predicted eruptive mass loss prevents stars of initial masses $\gtrsim20~M_\odot$ from evolving to become red supergiants, with the stars instead ending their lives as blue supergiants, and therefore offers a possible explanation for the observed lack of red supergiants in that mass regime. |
| title | A Model for Eruptive Mass Loss in Massive Stars |
| topic | Solar and Stellar Astrophysics Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2405.12274 |