| abstract: |
Debris disks are known to be a common feature around main-sequence stars.
Comprising solid material ranging from micron-sized dust to planetesimals of s everal km in radius, debris disks are the remnants of planet
formation. However, sensitive to observations is only the disks' dust
portion. This talk focusses on modeling such disk systems; in particular
two approaches are presented: the traditional modeling method and a new,
more elaborate one as proposed by Krivov et al. 2008. While the
traditional way simply assumes powerlaws for the emitting dust's spatial
and grain size distributions,the new approach provides a self-consistent
description of the dust and planetesimal distribution, paying more
attention to the dynamical processes at work in debris disks.
Applications to the debris disk systems of HR 8799 and Vega for the old
and new modeling approach, respectively, are discussed. |
