Dynamical simulation of the ``velocity-porosity'' reduction in observed strength of stellar wind lines

摘要: I use dynamical simulations of the line-driven instability to examine potential role resulting flow structure in reducing observed strength wind absorption lines. Instead porosity length formalism used model effects on continuum absorption, suggest reductions line can be better characterized terms a velocity clumping factor that is insensitive spatial scales. Examples dynamic spectra computed directly from do exhibit net reduction but only at modest 10-20% level well short ca. 10 required by recent analyses PV