- Dusty disks around young stars
- Award date
- 10 November 2009
- Number of pages
- Document type
- PhD thesis
- Faculty of Science (FNWI)
- Anton Pannekoek Institute for Astronomy (API)
Stars are formed through the collapse of giant molecular clouds. During this contraction the matter spins up and naturally forms a circumstellar disk. Once accretion comes to a halt, these disks are relatively stable. Some disks are known to last up to 10 Myrs. Most disks however, dissipate on shorter time scales under the influence of photoevaporation and planet formation. These disks, consisting of 99% gas and 1% dust, have revealed a high variety of dust composition and geometry. It is not clear what determines this variety and if higher mass stars also display this variety. In this thesis we analyzed a large sample of young stars, covering a mass range of ~2 to ~20 solar masses. Mid infrared imaging and spectroscopy have been obtained, to determine their composition and geometry. The results were placed in a multi-wavelength context as provided by the literature and a survey for any possible trends was carried out. In addition, case studies were performed of two special stars. Comprehensive data sets were gathered and a radiative transfer code was used to create detailed models of their disk geometry.
- Research conducted at: Universiteit van Amsterdam
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