Wind line variability and intrinsic errors in observational mass loss rates

TL;DR

This study quantifies the intrinsic variability in UV wind line profiles of OB stars and its impact on the accuracy of mass loss rate measurements, revealing significant uncertainties and wind structure implications.

Contribution

It provides a comprehensive analysis of wind line variability in OB stars and estimates the intrinsic errors in mass loss rates from single observations, highlighting temperature-dependent effects.

Findings

Mass loss rate measurements vary by about 22% RMS on average.

Variations can cause single measurements to differ by a factor of 2 or more.

Hotter stars show smaller optical depth variations, indicating different wind structures.

Abstract

UV wind line variability in OB stars appears to be universal. To quantify this variation and to estimate its effect on a mass loss rate determined from a single observation, we use the IUE archive to identify non-peculiar OB stars with well developed but unsaturated Si IV 1400 doublets and at least 10 independent observations. This resulted in 1699 spectra of 25 stars. We use SEI modelling to translate the profile variations into optical depth variations and, hence, variations in measured mass loss rates. These variations quantify the intrinsic error inherent in any mass loss rate derived from a single observation. The derived rates have an overall RMS variation of about 22%, but this differs with effective temperature, being as small at 8% for the hottest stars and up to 45% for the cooler ones. Furthermore, any single determination can differ from the mean by a factor of 2 or more. Our results also imply that mass loss rates determined from non-simultaneous observations (such as UV and ground based data) need not agree. We also use our results to examine the nature of the wind structures responsible for the variability. Our findings suggest that the optical depth variations result from optically very thick structures occulting more or less of the line of sight to the stellar disk. Further, the smaller optical depth variations in the hottest stars suggests that the responsible structures are disrupted in their more powerful winds.