Transitional And Pre-transitional Disks: Gap Opening By Multiple Planets?

Details Transitional And Pre-transitional Disks: Gap Opening By Multiple Planets? Transitional And Pre-transitional Disks: Gap Opening By Multiple Planets?

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21732203z&link_type=abstract

American Astronomical Society, AAS Meeting #217, #322.03; Bulletin of the American Astronomical Society, Vol. 43, 2011

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Scientific paper

We use two-dimensional hydrodynamic simulations of viscous disks to examine whether dynamically-interacting multiple giant planets can explain the large gaps inferred for the transitional and pre-transitional disks around T Tauri stars. In the absence of inner disk dust depletion, we find that it requires three to four giant planets to open up large enough gaps to be consistent with inferences from spectral energy distributions, because the gap width is limited by the tendency of the planets to be driven together into 2:1 resonances.With very strong tidal torques and/or rapid planetary accretion, fewer planets can also generate a large cavity interior to the locally formed gap(s) by preventing outer disk material from moving in. In these cases, however, the reduction of surface density produces a corresponding reduction in the inner disk accretion rate onto the star; this makes it difficult to explain the observed accretion rates of the pre/transitional disks. We find that even with planet(s) in disks, additional substantial dust depletion is required to explain observed disk gaps/holes. Substantial dust settling and growth, with consequent significant reductions in optical depths, is inferred for typical T Tauri disks in any case, and an earlier history of dust growth is consistent with the hypothesis that pre/transitional disks are explained by the presence of giant planets. We suggest that in the pre/transitional disks,giant planet formation modifies this general process by forming a gap with abrupt changes in surface density, producing a thick outer disk ``wall'' which can be strongly irradiated by the central star, while scattering and clearing inner planetesimals that otherwise might collide and produce secondary small dust.

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