  Hot massive stars exhibit strong stellar winds that enrich the surrounding
interstellar medium and affect the stars' evolution. However, the winds are
inhomogeneous (clumped) and are difficult to model in radiative transfer codes.
To produce more realistic spectra many codes use a volume-filling factor
approach to incorporate the effects of clumping. While this approach is
convenient it is simplistic. We introduce an alternative approach to
incorporate clumping by assuming the wind is composed of dense spherical
shells. Using this approach in the radiative transfer code CMFGEN we produce
synthetic spectra for AzV83, an O7Iaf+ supergiant located in the Small
Magellanic Cloud. The spectrum of AzV83 is rich in both photospheric and wind
features, making it an ideal candidate with which to investigate the physical
characteristics of stellar winds. Synthetic spectra are compared to the star's
observed spectrum to better characterize the influence of clumped winds on
spectral features, and to better understand the limitations of the
volume-filling factor approach. The approach using spherical shells yields
similar wind parameters to those obtained using the volume-filling factor
approach although a slightly higher mass-loss rate is required to fit
H$\alpha$. As expected, the interclump medium in the model with shells allows
the high ionisation resonance transitions of N V and O VI to be fitted using
$L_{\rm X-ray}/L_{\rm Bol} \approx 10^{-7}$ which is typically observed for O
stars, and which is a factor of ten lower than needed with the volume-filling
factor approach.
