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
