The Ionization in the Winds of O Stars and the Determination of Mass-loss Rates from Ultraviolet Lines

Empirical ionization fractions of C IV, N V, Si IV, and empirical ionization plus excitation fractions of C III* and N IV* in the winds of 34 O stars and one B star have been derived. We combine the mass-loss rates derived from radio measurements and Ha with the line Ðtting of ultraviolet resonance lines and subordinate lines using the Sobolev plus exact integration (SEI) method. The dependence of the empirical ionization fractions, SqT, on the stellar e†ective temperature and on the mean wind density is discussed. This sets constraints for the models of ionization in the winds of hot stars. The ionization and excitation fractions can be expressed in terms of an empirical radiation temperature. This radiation temperature scales with and we derive empirical relations for as a function of The radiation Teff, Trad Teff. temperatures are on the order of 0.5È0.9 with signiÐcant di†erences between the ions. The derived Teff, relations between the ionization fractions and the stellar parameters have an uncertainty of 0.2 dex for Si IV, N V, and C III*, and about 0.26 dex for N IV*. For C IV, we can only derive an expression for the mean ionization fraction in the wind if the mass-loss rate is small, yr~1, because the C IV M0 \ 10~6 M _ lines are usually saturated for higher mass-loss rates. The resulting expressions for can be used to Trad derive the mass-loss rates from studies of ultraviolet P Cygni proÐles in the range of stellar parameters studied here : 30,000 K, and [ 7.5 K [Teff [ 50,500 5.2[ log L /L * [ 6.4, M_[ log M0 [ [4.6 M_ yr~1. An accuracy of about a factor of 2 or better can be reached, depending on the lines that are used and the accuracy of the line Ðts and the stellar parameters. The Si IV lines give the most reliable massloss rates, because the abundance is about the same for all O stars, the lines saturate only for high mass-loss rates, the doublet lines only partly overlap, and the mass-loss rate is proportional to the square root of the column density. The radiation temperature of N V shows a surprisingly strict relation with with a scatter of only The mass-loss rate cannot be derived from the N V Teff, *Trad/Teff \ 0.01. lines, because the column density of the N V ions in the wind is independent of A consistency check M0 . and a test of the method for the stars HD 14749 and HD 190429 show that the mass-loss rate derived from the UV lines with the ionization fractions of this paper agree very well with the mass-loss rate derived from new radio Ñux measurements. Subject headings : stars : atmospheres È stars : early-type È stars : mass loss È ultraviolet : stars