2012A&A...544A.120L

A two-component phenomenological model developed originally for ζ Puppis is revised in order to model the outflows of late-type O dwarfs that exhibit the weak-wind phenomenon. With the theory's standard parameters for a generic weak-wind star, the ambient gas is heated to coronal temperatures ≃3x10⁶K at radii >1.4R, with cool radiation-driven gas being then confined to dense clumps with filling factor ≃0.02. Radiative driving ceases at radius ≃2.1R when the clumps are finally destroyed by heat conduction from the coronal gas. Thereafter, the outflow is a pure coronal wind, which cools and decelerates reaching ∞ with terminal velocity ≃1000km/s.