Dynamics and structure in resolved dusty disks

Details Dynamics and structure in resolved dusty disks Dynamics and structure in resolved dusty disks

Oct 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005nrdd.conf....2a&link_type=abstract

Proceedings of the Miniworkshop on Nearby Resolved Debris Disks. October 19-20, 2005. Space Telescope Science Institute, Baltimo

Physics

Scientific paper

Numerous ways in which stellar and planetary disks acquire observed structure through internal dynamics or interaction with embedded planets are reviewed. The structure is often found at large distances from a star, where the hypothetical giant planets cannot form through standard mechanism of core accretion. Outward migration of protoplanets may be the resolution of this problem.
Post-T Tau, transitional and beta Pic-type objects may exhibit interesting ringlike and nonaxisymmetric features due to coupling of dust and gas in the presence of stellar radiation. In particular, we discuss a new instability that can operate in optically thick and intermediate disks. Some of these structures are similar to those caused by the gravity of planets. Therefore, careful theoretical modeling is required for the correct interpretation of imaging data.

Affiliated with

Also associated with

No associations

Rating

Dynamics and structure in resolved dusty disks does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Dynamics and structure in resolved dusty disks, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Dynamics and structure in resolved dusty disks will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1382706