The ISO spectrum of the young star HD 142527

We present a detailed analysis of SWS (2.35-45 mu m) and LWS (43-200 mu m) spectra obtained with the Infrared Space Observatory (ISO) (Kessler et al. 1996) of the dusty circumstellar disk surrounding the isolated young Fe sta r HD 142527. Two dust populations can be clearly discriminated: a warm comp onent which is dominated by very strong silicate emission at 10 mu m, but i n which C-rich dust is observable as well, and a cool component, of which t he spectrum is dominated by O-rich dust features (C-rich dust not cause obv ious features in the far infrared). Besides silicates, crystalline water-ic e and hydrous silicates - which are also found in interplanetary dust parti cles - are present in the cold circumstellar environment. The ISO spectrum of HD 142527 differs markedly from that of HD 100546 (Malfait et al. 1998b) and other objects in a similar evolutionary stage and with a similar broad -band energy distribution. No clear correlations between the spectral dust signatures and the stellar parameters can be found at the present stage.