The nature and consequences of clumping in hot, massive star winds

2011/10/03 by J. O. Sundqvist, Sundqvist, Jon O., S. P. Owocki +3
Agricultural and Biological Sciences · Physics and Astronomy · #Astrophysics and Star Formation Studies #Bee Products Chemical Analysis #FOS: Physical sciences #Solar and Stellar Astrophysics (astro-ph.SR) #Stellar, planetary, and galactic studies

paper · pdf · doi:10.48550/arxiv.1110.0485

openalex publication_date 2011/10/03 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28

Abstract

This review describes the evidence for small-scale structure, `clumping', in the radiation line-driven winds of hot, massive stars. In particular, we focus on examining to what extent simulations of the strong instability inherent to line-driving can explain the multitude of observational evidence for wind clumping, as well as on how to properly account for extensive structures in density and velocity when interpreting the various wind diagnostics used to derive mass-loss rates.

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