Model infrared spectra of passively heated proto-planetary disks surrounding intermediate-mass pre-main-sequence stars

Aims. We study theoretical spectra at mid-infrared (5−40 μm) wavelengths of proto-planetary disks surrounding intermediate-mass pre-main-sequence stars. Observations show a wide range of spectral shapes and a rich variety in strength and shape of dust resonances. These strong variations in spectral shape reflect differences in the nature and spatial distribution of dust particles in the disk. The aim of this study is to establish what model parameters influence the mid-IR spectra of planet-forming disks. Methods. A grid of models of passively heated proto-planetary disks is used to calculate the infrared spectrum. We use hydrostatic equilibrium disk models and radiative transfer to calculate the emerging spectrum. We focus on the effects that different disk geometries (flaring, self-shadowed) and dust mineralogy have on the emerging 5−40 μm spectrum. We adopt four scenarios for the radial and vertical distribution of crystalline silicate dust. Results. In our model, the 23.5 μm forsterite band is more sensitive to emission from regions <30 AU, while the 33.5 μm forsterite band probes regions up to 50 AU. The 23.5 μm band strength does not depend on the degree of flaring of the disk, while the 33.5 μm band does. Only models with a substantial abundance (>5 percent) of crystalline silicates at a long distance from the star (>20−50 AU) show detectable emission in the 33.5 μm forsterite band. The carbon-dust abundance affects the strength of the dust resonances in the 10 μm spectral region, but not in the 30 μm region.