The winds of OBA hypergiants and luminous blue variables: Dynamically-consistent atmosphere models reveal multiple wind regimes
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2026
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| author | Bernini-Peron, Matheus Sander, Andreas A. C. Sabhahit, Gautham N. Najarro, Francisco Ramachandran, Varsha Vink, Jorick S. |
| author_facet | Bernini-Peron, Matheus Sander, Andreas A. C. Sabhahit, Gautham N. Najarro, Francisco Ramachandran, Varsha Vink, Jorick S. |
| contents | OBA hypergiants (OBAHGs) are evolved massive stars with notable wind features in their optical spectrum. Located at the cool edge of the line-driven wind regime, many are candidate luminous blue variables (LBVs) likely near the Eddington limit. Although brief, this evolutionary stage deeply affects their surroundings and subsequent evolution.
We study the mechanisms behind OBAHG winds and spectra, covering the temperature range of non-eruptive LBVs. Using the PoWR atmosphere code, we compute models with an Eddington parameter Gamma_e ~ 0.4 and moderate turbulent pressure, typical for cool hypergiants, varying the effective temperature from ~12.5 to ~38.0 kK at solar metallicity.
Our models show a complex temperature-dependent mass-loss pattern, with regions of higher/lower rates linked to two wind solutions: "dense" and "rarefied." Spectra of known OBAHGs and LBVs match models from all solution regions. We find bi-stability jumps -- with sharp mass-loss increases -- at temperatures where Fe IV recombines to Fe III (and Fe III to Fe II). "Drops" in mass loss also occur when the leading Fe ion changes at wind onset, signaling a switch to rarefied solutions under insufficient driving opacity.
The resulting velocity fields also reflect these different regimes: rarefied solutions match the empirical terminal velocity vs temperature relation, while dense ones deviate. Turbulent pressure is crucial for wind acceleration at cooler temperatures.
We demonstrate that the bi-stability jumps exist in OBAHGs but are part of a broader complex behavior not replicated by current mass-loss recipes. Combining our and other recent results, we suggest that the switch between rarefied and dense solutions only occurs within a certain proximity to the Eddington Limit. Testing this requires future models with broader parameters and advanced treatments of radiatively-driven turbulence. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2601_03072 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | The winds of OBA hypergiants and luminous blue variables: Dynamically-consistent atmosphere models reveal multiple wind regimes Bernini-Peron, Matheus Sander, Andreas A. C. Sabhahit, Gautham N. Najarro, Francisco Ramachandran, Varsha Vink, Jorick S. Solar and Stellar Astrophysics OBA hypergiants (OBAHGs) are evolved massive stars with notable wind features in their optical spectrum. Located at the cool edge of the line-driven wind regime, many are candidate luminous blue variables (LBVs) likely near the Eddington limit. Although brief, this evolutionary stage deeply affects their surroundings and subsequent evolution. We study the mechanisms behind OBAHG winds and spectra, covering the temperature range of non-eruptive LBVs. Using the PoWR atmosphere code, we compute models with an Eddington parameter Gamma_e ~ 0.4 and moderate turbulent pressure, typical for cool hypergiants, varying the effective temperature from ~12.5 to ~38.0 kK at solar metallicity. Our models show a complex temperature-dependent mass-loss pattern, with regions of higher/lower rates linked to two wind solutions: "dense" and "rarefied." Spectra of known OBAHGs and LBVs match models from all solution regions. We find bi-stability jumps -- with sharp mass-loss increases -- at temperatures where Fe IV recombines to Fe III (and Fe III to Fe II). "Drops" in mass loss also occur when the leading Fe ion changes at wind onset, signaling a switch to rarefied solutions under insufficient driving opacity. The resulting velocity fields also reflect these different regimes: rarefied solutions match the empirical terminal velocity vs temperature relation, while dense ones deviate. Turbulent pressure is crucial for wind acceleration at cooler temperatures. We demonstrate that the bi-stability jumps exist in OBAHGs but are part of a broader complex behavior not replicated by current mass-loss recipes. Combining our and other recent results, we suggest that the switch between rarefied and dense solutions only occurs within a certain proximity to the Eddington Limit. Testing this requires future models with broader parameters and advanced treatments of radiatively-driven turbulence. |
| title | The winds of OBA hypergiants and luminous blue variables: Dynamically-consistent atmosphere models reveal multiple wind regimes |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2601.03072 |