[Previous] | [Session 93] | [Next]
A. Li, J.I. Lunine, G.J. Bendo (University of Arizona)
We model the infrared (IR) emission from protoplanetary dust disks in terms of highly porous cometary-type dust made either of coagulated but otherwise unaltered protostellar interstellar grains, or grains that are highly-processed in protostellar/protoplanetary nebulae with silicate dust annealed and carbon dust oxidized. It is shown that the porous dust model with a vacuum volume fraction of ~ 90% is successful in reproducing the near-IR to submillimeter spectral energy distributions and the mid-IR spectral features of amorphous and/or crystalline silicate dust and polycyclic aromatic hydrocarbon molecules, as well as the images of scattered starlight, mid-IR and/or submillimeter dust thermal emission from six archetypal dust disks: HR 4796A (Li & Lunine 2003, ApJ, 590, 368), HD 141569A (Li & Lunine 2003, ApJ, 594, 987), \beta Pictoris (Li & Greenberg 1998, A&A, 331, 291), \epsilon Eridani (Li, Lunine, & Bendo, 2003, ApJL, in press), Fomalhaut and Vega (Li, Lunine, & Bendo, 2003, in preparation).
The author(s) of this abstract have provided an email address for comments about the abstract: agli@lpl.arizona.edu
[Previous] | [Session 93] | [Next]
Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.