Our ability to correct the observational photometry of galaxies depends upon our knowledge of the attenuation of light produced by the dust contained in the interstellar medium. I will present a model based on the statistical properties of the local density in isothermal turbulence which might be appropriate to study the radiative transport through the diffuse interstellar medium. The model will be applied to study the attenuation caused by a distant foreground screen and a non scattering slab where the sources are mixed within the turbulent medium. I will show how the turbulent structure effects the attenuation curve and how the attenuation curve varies with the thickness of a foreground screen.