We investigate the radiative transfer of Lyα photons through simplified anisotropic gas distributions, which represent physically motivated extensions of the popular shell models. Our study is motivated by the notion that (i) shell models do not always reproduce observed Lyα spectral line profiles; (ii) (typical) shell models do not allow for the escape of ionizing photons; and (iii) the observation and expectation that winds are more complex, anisotropic phenomena. We examine the influence of inclination on the Lyα spectra, relative fluxes and escape fractions. We find the flux to be enhanced/suppressed by factors up to a few depending on the parameter range of the models, corresponding to a boost in equivalent width of the same amplitude if we neglect dust. In general, lower mean optical depths tend to reduce the impact of anisotropies as is expected. We find a correlation between an observed peak in the – occasionally triple-peaked – spectrum at the systemic velocity and the existence of a low optical depth cavity along the line of sight. This can be of importance in the search for ionizing photons leaking from high- redshift galaxies since these photons will also be able to escape through the cavity.