Grain growth in the inner regions of Herbig Ae/Be star disks

Details Grain growth in the inner regions of Herbig Ae/Be star disks Grain growth in the inner regions of Herbig Ae/Be star disks

Mar 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003a%26a...400l..21v&link_type=abstract

Astronomy and Astrophysics, v.400, p.L21-L24 (2003)

Astronomy and Astrophysics

Astrophysics

130

Stars: Circumstellar Matter, Stars: Pre-Main-Sequence, Infrared: Ism: Lines And Bands

Scientific paper

We present new mid-infrared spectroscopy of the emission from warm circumstellar dust grains in Herbig Ae/Be stars. Our survey significantly extends the sample that was studied by Bouwman et al. (2001). We find a correlation between the strength of the silicate feature and its shape. We interpret this as evidence for the removal of small (0.1 mu m) grains from the disk surface while large (1-2 mu m) grains persist. If the evolution of the grain size distribution is dominated by gravitational settling, large grains are expected to disappear first, on a timescale which is much shorter than the typical age of our programme stars. Our observations thus suggest a continuous replenishment of micron sized grains at the disk surface. If the grain replenishment is due to the dredge-up of dust from the disk interior, the mineralogy we observe is representative of the bulk composition of dust in these stars.
Based on observations obtained at the European Southern Observatory (ESO), La Silla, and on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, The Netherlands and the UK) and with the participation of ISAS and NASA.

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