New self-consistent theoretical descriptions for mass-loss rates of O-type stars

February 18, 2026

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This research aims to develop accurate models for predicting mass-loss rates of O-type stars, influencing their evolution and impact on the interstellar medium.
Computed wind parameters for O-type stars using a self-consistent approach.
Coupled hydrodynamics of the wind with line acceleration calculations.
Utilized tailored non-local thermodynamic equilibrium models as input for radiation fields.
Iteratively solved wind hydrodynamics until convergence across various stellar parameters.
Obtained self-consistent wind parameters for diverse O-type stellar models.
Observed systematic decrease in mass-loss rates with increased elements in the radiation field.
Achieved high Pearson correlation values (>0.92) for theoretical prescriptions and estimated wind momentum-luminosity relationships.

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Models compute mass-loss rates in O-type stars, revealing effects of element inclusion on UV radiation.

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Figueroa-Tapia et al. (2026) studied this question.

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