Ion Fractions and the Weak Wind Problem

Details Ion Fractions and the Weak Wind Problem Ion Fractions and the Weak Wind Problem

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011bsrsl..80..120a&link_type=abstract

Société Royale des Sciences de Liège, Bulletin, vol. 80, p. 120-124 (Proceedings of the 39th Liège Astrophysical Colloquium, hel

Statistics

Computation

Scientific paper

Some late-type O stars are observed to display anomalously weak winds. This issue and the uncertainty about the nature of wind clumping are challenges to line-driven wind theory and need resolving in order to fully understand hot stars. We describe the results from the computation of ion fractions for the various elements in O star winds using the non-LTE code CMFGEN, including parameterisations of microclumping and X-rays. Ion fractions can also be derived from fits to UV wind lines if a mass-loss rate is assumed. We discuss a project to fit unsaturated C IV lines in late O dwarfs, and show that the weak wind scenario could still be a major issue, with some values of dot{M}< q_{C IV} > indicated to be more than an order of magnitude lower than theoretical predictions of mass-loss, and measurements from radio and optical diagnostics.

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