Probing the inner accretion disk using Spitzer c2d mid-infrared spectra

Details Probing the inner accretion disk using Spitzer c2d mid-infrared spectra Probing the inner accretion disk using Spitzer c2d mid-infrared spectra

Jul 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007sf2a.conf..541o&link_type=abstract

SF2A-2007: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics held in Grenoble, France, July

Astronomy and Astrophysics

Astrophysics

Scientific paper

Mid-infrared emission from silicates grains around young stars arises from the inner disks regions (at distances smaller than a few AU), and can serve to probe the dust content and disk structure close to the inner disk edge. We obtained more than a hundred of Spitzer/IRS spectra in a 5-35 μm range, as part of the Cores to Disks (c2d) Legacy Program. The sample consists of mostly Class II objects (T Tauri) and they all show silicate emission features. In addition, a large fraction of them (˜ 80%, Olofsson et al. in prep) show at least one crystalline silicate feature which could be attributed to crystalline Mg-rich silicates (forsterite or enstatite) or other crystalline components (diopside, etc). A statistical study, led by Kessler-Silacci et al. (2006, 2007), evidenced a correlation between the spectral type of the central star and the silicate grain size. This correlation finds an explanation considering the illumination from the star (the 10 μm emission zone is closer to the star for less luminous sources; less than a tenth of AU for a star luminosity smaller than ˜ 0.01 L&odotB}) and by the fact that the grains are, on average, expected to be larger at smaller radii. These results were obtained using the CGPlus two-layer disk model, therefore only geometrical considerations were studied. Future modelling including more details of grain coagulation, thermal processing and accretion events will be needed to strengthen this study. But the complexity of such modelling is beyond the scope of this poster.

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