Other
Scientific paper
Sep 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.1308y&link_type=abstract
American Astronomical Society, DPS meeting #38, #13.08; Bulletin of the American Astronomical Society, Vol. 38, p.506
Other
Scientific paper
One of the unsolved issues in planetary system formation is how kilometer-sized planetesimals form. The fragmentation of the dust layer due to gravitational instability (hereafter referred GI) is one of possible models. We investigate the density evolution in the dust layer of a protoplanetary disk due to the GI and dust settling toward the midplane. We restrict to consider the region where the radial pressure gradient at equilibrium is negligible so that the shear-induced instability is avoided, and we also restrict our model to an axisymmetric perturbation as a first step of nonlinear numerical simulations of the GI. We show that there are two different evolutionary paths of the GI, depending on the nondimensional gas friction time, which is defined as the product of the gas friction time and the Keplerian angular velocity. If the nondimensional gas friction time is equal to 0.01, the GI grows faster than dust settling. On the other hand, if the nondimensional gas friction time is equal to 0.1, dust aggregates settle sufficiently before the GI grows. In the latter case, an approximate analytical calculation reveals that dust settling is faster than the growth of the GI, regardless of the dust density at the midplane. Thus, the dust layer becomes extremely thin and may reach a few tenths of the material density of the dust before the GI grows, as long as there is no turbulence. In order to elucidate whether the planetesimal formation due to the GI is possible or not, we plan to perform nonaxisymmetric simulations in the future. This work was supported by JSPS Research Fellowship for Young Scientists and Grants-in-Aid from the Japanese Ministry of Education, Culture, Sports, Science, and Technology.
Sekiya Minoru
Yamoto Fumiharu
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