New self-consistent theoretical descriptions for mass-loss rates of O-type stars
- Autores
- Figueroa-Tapia, F.; Panei, Jorge Alejandro; Curé, M.; Araya, I.; Ekström, S.; Gormaz-Matamala, A. C.; Venero, Roberto Oscar José; Cidale, Lydia Sonia
- Año de publicación
- 2026
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Context. Massive O-type stars lose a significant fraction of their mass through radiation-driven winds, a process that critically shapes their evolution and feedback into the interstellar medium. Accurate predictions of mass-loss rates ( Ṁ) are essential for models of stellar structure and population synthesis. Aims. We computed wind parameters for O-type stars using a self-consistent approach that couples the hydrodynamics of the wind with detailed calculations of the line acceleration. This approach follows the theory of radiation-driven stellar winds and, thus, allows us to derive mass-loss rate distributions for different atomic configurations of the stellar flux. Methods. We used the TLUSTY code for stellar atmosphere models to compute tailored non-local thermodynamic equilibrium mod- els; these models served as input radiation fields for the calculation of the force multiplier factor and the line-force parameters, for which we used the LOCUS code. These line-force parameters were then iteratively coupled with the HYDWIND code to solve the wind hydrodynamics. The procedure was repeated until convergence and applied across a grid of stellar parameters for three chemical configurations. Results. We obtain self-consistent wind parameters for a broad set of O-type stellar models. The results show a systematic decrease in mass-loss rates with the inclusion of more elements in the radiation field, which is attributed to a strong effect on the UV region of the spectral energy distribution. As more elements are included, resulting in a larger number of spectral lines, the contribution from the UV diminishes, leading to lower mass-loss rates. We fitted three theoretical prescriptions for Ṁ using a Bayesian approach; this yielded Pearson correlation values greater than 0.92 for all three model grids. It also allowed for the estimation of the wind momentum-luminosity relationships for each of the grids, yielding results similar to those based on observations of O-type stars.
Instituto de Astrofísica de La Plata - Materia
-
Ciencias Astronómicas
Stars: atmospheres
Stars: massive
Stars: mass-loss
Stars: winds, outflows - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by/4.0/
- Repositorio
.jpg)
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/195626
Ver los metadatos del registro completo
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New self-consistent theoretical descriptions for mass-loss rates of O-type starsFigueroa-Tapia, F.Panei, Jorge AlejandroCuré, M.Araya, I.Ekström, S.Gormaz-Matamala, A. C.Venero, Roberto Oscar JoséCidale, Lydia SoniaCiencias AstronómicasStars: atmospheresStars: massiveStars: mass-lossStars: winds, outflowsContext. Massive O-type stars lose a significant fraction of their mass through radiation-driven winds, a process that critically shapes their evolution and feedback into the interstellar medium. Accurate predictions of mass-loss rates ( Ṁ) are essential for models of stellar structure and population synthesis. Aims. We computed wind parameters for O-type stars using a self-consistent approach that couples the hydrodynamics of the wind with detailed calculations of the line acceleration. This approach follows the theory of radiation-driven stellar winds and, thus, allows us to derive mass-loss rate distributions for different atomic configurations of the stellar flux. Methods. We used the TLUSTY code for stellar atmosphere models to compute tailored non-local thermodynamic equilibrium mod- els; these models served as input radiation fields for the calculation of the force multiplier factor and the line-force parameters, for which we used the LOCUS code. These line-force parameters were then iteratively coupled with the HYDWIND code to solve the wind hydrodynamics. The procedure was repeated until convergence and applied across a grid of stellar parameters for three chemical configurations. Results. We obtain self-consistent wind parameters for a broad set of O-type stellar models. The results show a systematic decrease in mass-loss rates with the inclusion of more elements in the radiation field, which is attributed to a strong effect on the UV region of the spectral energy distribution. As more elements are included, resulting in a larger number of spectral lines, the contribution from the UV diminishes, leading to lower mass-loss rates. We fitted three theoretical prescriptions for Ṁ using a Bayesian approach; this yielded Pearson correlation values greater than 0.92 for all three model grids. It also allowed for the estimation of the wind momentum-luminosity relationships for each of the grids, yielding results similar to those based on observations of O-type stars.Instituto de Astrofísica de La Plata2026-02info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/195626enginfo:eu-repo/semantics/altIdentifier/issn/1432-0746info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202558657info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by/4.0/Creative Commons Attribution 4.0 International (CC BY 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2026-06-23T11:17:06Zoai:sedici.unlp.edu.ar:10915/195626Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292026-06-23 11:17:06.923SEDICI (UNLP) - Universidad Nacional de La Platafalse |
| dc.title.none.fl_str_mv |
New self-consistent theoretical descriptions for mass-loss rates of O-type stars |
| title |
New self-consistent theoretical descriptions for mass-loss rates of O-type stars |
| spellingShingle |
New self-consistent theoretical descriptions for mass-loss rates of O-type stars Figueroa-Tapia, F. Ciencias Astronómicas Stars: atmospheres Stars: massive Stars: mass-loss Stars: winds, outflows |
| title_short |
New self-consistent theoretical descriptions for mass-loss rates of O-type stars |
| title_full |
New self-consistent theoretical descriptions for mass-loss rates of O-type stars |
| title_fullStr |
New self-consistent theoretical descriptions for mass-loss rates of O-type stars |
| title_full_unstemmed |
New self-consistent theoretical descriptions for mass-loss rates of O-type stars |
| title_sort |
New self-consistent theoretical descriptions for mass-loss rates of O-type stars |
| dc.creator.none.fl_str_mv |
Figueroa-Tapia, F. Panei, Jorge Alejandro Curé, M. Araya, I. Ekström, S. Gormaz-Matamala, A. C. Venero, Roberto Oscar José Cidale, Lydia Sonia |
| author |
Figueroa-Tapia, F. |
| author_facet |
Figueroa-Tapia, F. Panei, Jorge Alejandro Curé, M. Araya, I. Ekström, S. Gormaz-Matamala, A. C. Venero, Roberto Oscar José Cidale, Lydia Sonia |
| author_role |
author |
| author2 |
Panei, Jorge Alejandro Curé, M. Araya, I. Ekström, S. Gormaz-Matamala, A. C. Venero, Roberto Oscar José Cidale, Lydia Sonia |
| author2_role |
author author author author author author author |
| dc.subject.none.fl_str_mv |
Ciencias Astronómicas Stars: atmospheres Stars: massive Stars: mass-loss Stars: winds, outflows |
| topic |
Ciencias Astronómicas Stars: atmospheres Stars: massive Stars: mass-loss Stars: winds, outflows |
| dc.description.none.fl_txt_mv |
Context. Massive O-type stars lose a significant fraction of their mass through radiation-driven winds, a process that critically shapes their evolution and feedback into the interstellar medium. Accurate predictions of mass-loss rates ( Ṁ) are essential for models of stellar structure and population synthesis. Aims. We computed wind parameters for O-type stars using a self-consistent approach that couples the hydrodynamics of the wind with detailed calculations of the line acceleration. This approach follows the theory of radiation-driven stellar winds and, thus, allows us to derive mass-loss rate distributions for different atomic configurations of the stellar flux. Methods. We used the TLUSTY code for stellar atmosphere models to compute tailored non-local thermodynamic equilibrium mod- els; these models served as input radiation fields for the calculation of the force multiplier factor and the line-force parameters, for which we used the LOCUS code. These line-force parameters were then iteratively coupled with the HYDWIND code to solve the wind hydrodynamics. The procedure was repeated until convergence and applied across a grid of stellar parameters for three chemical configurations. Results. We obtain self-consistent wind parameters for a broad set of O-type stellar models. The results show a systematic decrease in mass-loss rates with the inclusion of more elements in the radiation field, which is attributed to a strong effect on the UV region of the spectral energy distribution. As more elements are included, resulting in a larger number of spectral lines, the contribution from the UV diminishes, leading to lower mass-loss rates. We fitted three theoretical prescriptions for Ṁ using a Bayesian approach; this yielded Pearson correlation values greater than 0.92 for all three model grids. It also allowed for the estimation of the wind momentum-luminosity relationships for each of the grids, yielding results similar to those based on observations of O-type stars. Instituto de Astrofísica de La Plata |
| description |
Context. Massive O-type stars lose a significant fraction of their mass through radiation-driven winds, a process that critically shapes their evolution and feedback into the interstellar medium. Accurate predictions of mass-loss rates ( Ṁ) are essential for models of stellar structure and population synthesis. Aims. We computed wind parameters for O-type stars using a self-consistent approach that couples the hydrodynamics of the wind with detailed calculations of the line acceleration. This approach follows the theory of radiation-driven stellar winds and, thus, allows us to derive mass-loss rate distributions for different atomic configurations of the stellar flux. Methods. We used the TLUSTY code for stellar atmosphere models to compute tailored non-local thermodynamic equilibrium mod- els; these models served as input radiation fields for the calculation of the force multiplier factor and the line-force parameters, for which we used the LOCUS code. These line-force parameters were then iteratively coupled with the HYDWIND code to solve the wind hydrodynamics. The procedure was repeated until convergence and applied across a grid of stellar parameters for three chemical configurations. Results. We obtain self-consistent wind parameters for a broad set of O-type stellar models. The results show a systematic decrease in mass-loss rates with the inclusion of more elements in the radiation field, which is attributed to a strong effect on the UV region of the spectral energy distribution. As more elements are included, resulting in a larger number of spectral lines, the contribution from the UV diminishes, leading to lower mass-loss rates. We fitted three theoretical prescriptions for Ṁ using a Bayesian approach; this yielded Pearson correlation values greater than 0.92 for all three model grids. It also allowed for the estimation of the wind momentum-luminosity relationships for each of the grids, yielding results similar to those based on observations of O-type stars. |
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2026 |
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2026-02 |
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