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.
ÒporosityÓ) certainly could play a
role in the overall reduction of
wind optical depth.
N K-edge