  Motivated by recent detections by the XMM and Chandra satellites of X-ray
line emission from hot, luminous stars, we present synthetic line profiles for
X-rays emitted within parameterized models of a hot-star wind. The X-ray line
emission is taken to occur at a sharply defined co-moving-frame resonance
wavelength, which is Doppler-shifted by a stellar wind outflow parameterized by
a `beta' velocity law, $v(r)=v_{\infty} (1-\R_{\ast}/r)^\beta$. Above some
initial onset radius $R_o$ for X-ray emission, the radial variation of the
emission filling factor is assumed to decline as a power-law in radius, $f(r)
\sim r^{-q}$. The computed emission profiles also account for continuum
absorption within the wind, with the overall strength characterized by a
cumulative optical depth $\tau_\ast$. In terms of a wavelength shift from
line-center scaled in units of the wind terminal speed $v_{\infty}$, we present
normalized X-ray line profiles for various combinations of the parameters
$\beta$, $\tau_\ast$, $q$ and $R_o$, and including also the effect of
instrumental broadening as characterized by a Gaussian with a parameterized
width $\sigma$. We discuss the implications for interpreting observed hot-star
X-ray spectra, with emphasis on signatures for discriminating between
``coronal'' and ``wind-shock'' scenarios. In particular, we note that in
profiles observed so far the substantial amount of emission longward of line
center will be difficult to reconcile with the expected attenuation by the wind
and stellar core in either a wind-shock or coronal model.
