... for WNE

Early WN stars, WN2-5.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... Galaxy

Note that these numbers represent one possible random realisation of the model for a population of He+c.o. systems, so all numbers given are subject to Poisson noise.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... WR phenomenon

A possible reason for the absence of the WR phenomenon in low-mass He stars is that, for luminosity-to-mass ratios characteristic for them, one does not expect radial pulsations that may drive shock waves with a consequential increase in the gas density necessary to produce radiative stellar winds (see, e.g., Fadeyev & Novikova 2003).

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... wind-fed

Note that the estimate of $\dot{M}$ quoted above is more than an order of magnitude lower than would be expected for such a massive WR star, even when keeping in mind the low metallicity of IC10: $Z/Z_\odot \approx 0.25$ (e.g., Lequeux et al. 1979).

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.