O-star mass-loss rates at low metallicity

TL;DR

This study compares theoretical and observed mass-loss rates of extragalactic O stars at low metallicity, revealing significant discrepancies likely due to wind-clumping and suggesting possible unknown mass-loss mechanisms.

Contribution

It provides new calculations of mass-loss rates at low metallicity and discusses potential additional mechanisms beyond radiation-driven winds.

Findings

Theoretical and observed rates agree for early-type O stars.

Discrepancies for late-type O stars suggest overestimated observed rates.

Computed rates show non-power-law metallicity dependence.

Abstract

Mass fluxes J are computed for the extragalactic O stars investigated by Tramper et al. (2011; TSKK). For one early-type O star, computed and observed rates agree within errors. However, for two late-type O stars, theoretical mass-loss rates underpredict observed rates by ~ 1.6 dex, far exceeding observational errors. A likely cause of the discrepancy is overestimated observed rates due to the neglect of wind-clumping. A less likely but intriguing possibility is that, in observing O stars with Z/Z_sun ~ 1/7, TSKK have serendipitously discovered an additional mass-loss mechanism not evident in the spectra of Galactic O stars with powerful radiation-driven winds. Constraints on this unknown mechanism are discussed. In establishing that the discrepancies, if real, are inescapable for purely radiation-driven winds, failed searches for high-J solutions are reported and the importance of a numerical technique that cannot spuriously create or destroy momentum stressed. The Z-dependences of the computed rates for Z/Z_sun in the interval (1/30, 2) show significant departures from a single power law, and these are attributed to curve-of-growth effects in the differentially-expanding reversing layers. The best-fitting power-law exponents range from 0.68-0.97.