  The Chandra and XMM-Newton X-ray telescopes have led to numerous advances in
the study and understanding of astrophysical X-ray sources. Particularly
important has been the much increased spectral resolution of modern X-ray
instrumentation. Wind-broadened emission lines have been spectroscopically
resolved for many massive stars. This contribution reviews approaches to the
modeling of X-ray emission line profile shapes from single stars, including
smooth winds, winds with clumping, optically thin versus thick lines, and the
effect of a radius-dependent photoabsorption coefficient.
