An extensive grid of mass fluxes for Galactic O stars

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.