| Issue |
A&A
Volume 524, December 2010
|
|
|---|---|---|
| Article Number | A41 | |
| Number of page(s) | 7 | |
| Section | Stellar atmospheres | |
| DOI | https://doi.org/10.1051/0004-6361/201014784 | |
| Published online | 22 November 2010 | |
An extensive grid of mass fluxes for Galactic O stars
Astrophysics Group, Blackett LaboratoryImperial College London,
Prince Consort
Road,
London
SW7 2AZ,
UK
e-mail: l.lucy@imperial.ac.uk
Received: 13 April 2010
Accepted: 8 September 2010
A previously-described code for constructing moving reversing layers (MRL) is improved by replacing a two-parameter model for gl(v), the radiative acceleration due to lines, with a flexible non-parametric description, thus allowing a greater degree of dynamical consistency in modelling turbulent transonic flow in the outer atmospheric layers of O stars. With this new code, mass fluxes J are computed at fifty-seven points in (Teff,g)-space. Specifically, J’s are computed for all Lanz-Hubeny (2003) NLTE atmospheres with Teff(kK) ∈ (27.5,55) and log g(cms-2) ≤ 4.5. Differences with widely-used mass-loss formulae are emphasized, and opportunities for differential spectroscopic tests identified.
Key words: stars: early-type / stars: mass-loss / stars: winds, outflows
© ESO, 2010
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