P V and the Mass Loss Discrepancy in O Stars
Astrophysics
2007-05-23 v1
Abstract
Building upon a previous analysis of P V wind lines in LMC O stars, we analyze the P V wind lines in a sample of Galactic O stars which have empirical mass loss rates determined from either their radio fluxes or H alpha profiles. Since the wind analysis provides a measure of \dot{M}q where q is the ionization fraction of the ion, we determine q(P V) observationally. In spite of model predictions that q should be about 1 for mid-O stars, we find q(P V) is less than 0.15 throughout the O stars. We discuss the origin of this discrepancy.
Cite
@article{arxiv.astro-ph/0410089,
title = {P V and the Mass Loss Discrepancy in O Stars},
author = {D. Massa and A. W. Fullerton and R. K. Prinja},
journal= {arXiv preprint arXiv:astro-ph/0410089},
year = {2007}
}
Comments
3 pages, 1 figure; To appear in proceedings of conference "Astrophysics in the Far Ultraviolet: Five Years of Discovery with FUSE", ASP Conf. Series (ed. Sonneborn, Moos, & Andersson)