Note:
dotted line is interstellar.
Wind opacity for canonical B star abundances.
We
do expect some wavelength dependence
of the cross sections (and thus of
the wind optical depth), BUT
the lines we fit cover only
a modest range of wavelengths. And in the case of z
Pup, nitrogen overabundance (not
in calculation shown at right) could
flatten out the wavelength dependence
even more.
OR
perhaps clumping plays a role. And clumping (alt. “porosity”) certainly could play a role in the overall reduction of wind optical depth.
N K-edge
