A debris disk is a circumstellar disk of dust created by the collisions of planets and/or minor bodies such as asteroids. Because the emission and scattered light properties of dust are more easily observable than the planets themselves, these debris disks provide an indirect means to study planets and planet formation. Indeed, the dynamics of a planet interacting with the dust in a debris disk may sculpt it into elegant forms that reveal the planet, such as has been suggested for disk surrounding Vega.
Some of these debris disk systems are close enough that we can study them spatially and in great detail; these are the nearby resolved debris disks. Among them are the Fabulous Four, Vega, Fomalhaut, Beta Pictoris and Epsilon Eridani which were all detected by IRAS. Other more recently discovered sources include HR4796A, AU Mic, HD 141569 and HD107146. Since their discoveries, Spitzer, HST, Keck, Gemini and VLT data are providing a wealth of new data on these nearby resolved debris disks.
The goal of our workshop is to discuss these data as a whole set and to compare the data with models of their dynamics, radiative transfer and chemical/dust processed evolution. Topics we plan to address in this forum are:
- The complete inventory of currently known nearby, resolved debris disk systems
- The structure of these disks and their implied dynamical history
- The composition of the dust and its associated radiative transfer
- The role of the central star in shaping debris disks
- Evidence for the presence of planets in these systems
- The nature and origin of these systems: left over debris or failed planetary systems?
|Pawel Artymowicz||Kate Su|
|Jane Greaves||Taku Takeuchi|
|Paul Kalas||Alycia Weinberger|
|David Koerner||Mark Wyatt|
Workshop Organizing Committee
|Mark Clampin||Steve Lubow|
|David Golimowski||Margaret Meixner|
|Inga Kamp||Jeff Valenti|