Structure and composition of disks surrounding Herbig Be stars

Details Structure and composition of disks surrounding Herbig Be stars Structure and composition of disks surrounding Herbig Be stars

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008sptz.prop50180v&link_type=abstract

Spitzer Proposal ID #50180

Physics

Scientific paper

Infrared spectroscopy of proto-planetary disks using Spitzer IRS has in recent years provided a wealth of new insight into the physical and chemical processes that alter the warm dust located in the surface layers of these disks. Both grain growth and crystallization have been firmly established, and are interpreted as signposts of disk dissipation and possibly planet formation. One of the biggest surprizes of the Spitzer legacy so far is that very similar changes in grain properties occur over a wide range of central star mass (luminosity), from very low mass stars to Herbig Ae and late Be type stars. Grain processing thus does not seem to be related to central star properties, but is governed by the physical and chemical processes in the disk. Evidence is growing that also more massive stars may form through disk accretion and may have planets. We wish to establish the nature of the grains surrounding a carefully selected sample of massive Herbig Be stars in the 3-10 solar mass range, largely missed in all previous surveys. These observations will be an important addition to the spectral legacy of Spitzer. The data will allow us to establish up to which mass range grain processing occurs similar to lower mass young stars, and place disk processing and planet formation into the wider context of massive star formation.

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