Astronomy and Astrophysics – Astrophysics
Scientific paper
May 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dda....41.1004m&link_type=abstract
American Astronomical Society, DDA meeting #41, #10.04; Bulletin of the American Astronomical Society, Vol. 41, p.938
Astronomy and Astrophysics
Astrophysics
Scientific paper
The recent development of a new minimum mass solar nebula, under the assumption that the giant planets formed in the compact configuration of the Nice model, has shed new light on planet formation in the Solar System. Desch (2007) previously found that a steady state protoplanetary disk that has an outer boundary formed from photoevaporation by an external massive star would have a steep surface density profile. In a completely novel way, we have adapted numerical methods for solving propagating phase change problems to astrophysical disks. We find that a 1-D time-dependent disk model that self-consistently tracks the location of the outer boundary produces shallower profiles than those predicted for a steady state disk. The resulting surface density profiles have a radial dependence of Σ(r) α r(-1.012±0.008) that increases slowly with time to a value of ˜Σ (r) α r(-1.5). The evolutionary timescales of the model disks can be sped up or slowed down by altering the amount of FUV flux or the viscosity parameter α. Slowing the evolutionary timescale by decreasing the incident FUV flux can help to grow planets more rapidly, but at the cost of decreased migration timescales. In contrast, decreasing the strength of the viscosity allows for increased growth rates without significantly altering migration timescales. These disks are all characterized by outward mass transport, mass loss at the outer edge and a truncated outer boundary. The transport of mass from small to large radii can potentially prevent the rapid inward migration of Jupiter and Saturn, while at the same time supply enough mass to the outer regions of the disk for the formation of Uranus.
Mitchell Tyler R.
Stewart Glen Robert
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