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- W2000307147 abstract "We have determined accurate values of the product of the mass-loss rate and the ion fraction of P+4, q(P+4), for a sample of 40 Galactic O-type stars by fitting stellar wind profiles to observations of the P V resonance doublet obtained with FUSE, ORFEUS BEFS, and Copernicus. When P+4 is the dominant ion in the wind [i.e., 0.5 ≲ q(P+4) ≤ 1], q(P+4) approximates the mass-loss rate to within a factor of ≲2. Theory predicts that P+4 is the dominant ion in the winds of O7-O9.7 stars, although an empirical estimator suggests that the range O4-O7 may be more appropriate. However, we find that the mass-loss rates obtained from P V wind profiles are systematically smaller than those obtained from fits to Hα emission profiles or radio free-free emission by median factors of ~130 (if P+4 is dominant between O7 and O9.7) or ~20 (if P+4 is dominant between O4 and O7). These discordant measurements can be reconciled if the winds of O stars in the relevant temperature range are strongly clumped on small spatial scales. We use a simplified two-component model to investigate the volume filling factors of the denser regions. This clumping implies that mass-loss rates determined from ρ2 diagnostics have been systematically overestimated by factors of 10 or more, at least for a subset of O stars. Reductions in the mass-loss rates of this size have important implications for the evolution of massive stars and quantitative estimates of the feedback that hot-star winds provide to their interstellar environments." @default.
- W2000307147 created "2016-06-24" @default.
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- W2000307147 date "2006-02-01" @default.
- W2000307147 modified "2023-10-06" @default.
- W2000307147 title "The Discordance of Mass‐Loss Estimates for Galactic O‐Type Stars" @default.
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- W2000307147 doi "https://doi.org/10.1086/498560" @default.
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