Macroclumping as solution of the discrepancy between Hαand P v mass loss diagnostics for O-type stars

2013/10/01 by B. Šurlan, W. -R. Hamann, W.-R. Hamann +4 · 1 citation
Physics and Astronomy · Social Sciences · #Astronomical spectroscopy #Astronomy and Astrophysical Research #Educational Leadership and Practices #Hertzsprung–Russell diagram #O-type star #Resonance (particle physics) #Spectral line #Stars #Stellar atmosphere #Stellar wind #Stellar, planetary, and galactic studies #astro-ph.SR

paper · pdf · doi:10.1051/0004-6361/201322390

published as Astronomy and Astrophysics, Volume 559, id.A130, 17 pp (2013) · 18 pages, 14 figures, 5 tables, accepted for publication in Astrononomy & Astrophysics

arxiv created 2013/10/01 · openalex publication_date 2013/10/18 · arxiv updated 2014/06/16 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05

Abstract

Context. Recent studies of O-type stars have demonstrated that discrepant mass-loss rates are obtained when different diagnostic methods are employed. Fitting the unsaturated UV resonance lines (e.g., P v) gives drastically lower values than obtained from the Hα emission. Wind inhomogeneity (so-called “clumping”) may be the main cause of this discrepancy.

Citations

• On the Importance of the Interclump Medium for Superionization: O vi Formation in the Wind of ζ Puppis
• Neglecting the porosity of hot-star winds can lead to underestimating mass-loss rates
• The chemical composition of the Sun

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