Computer Science
Scientific paper
Jul 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004sosyr..38..288m&link_type=abstract
Solar System Research, v. 38, Issue 4, p. 288-300 (2004).
Computer Science
2
Scientific paper
We consider the formation of cometlike and larger bodies in the trans-Neptunian region of the protoplanetary gas-dust disk. Once the particles have reached 1-10 cm in size through mutual collisions, they compact and concentrate toward the midplane of the disk to form a dust subdisk there. We show that after the subdisk has reached a critical density, its inner, equatorial layer that, in contrast to the two subsurface layers, contains no shear turbulence can be gravitationally unstable. The layer breaks up into ~1012-cm clumps whose small fragments (~109 cm) can rapidly contract to form bodies ~10 km in size. We consider the sunward drift of dust particles at a velocity that decreases with decreasing radial distance as the mechanism of radial contraction and compaction of the layer that contributes to its gravitational instability and the formation of larger (~100 km) planetesimals. Given all of the above processes, it takes ~106 yr for planetesimals to form, which is an order of magnitude shorter than the lifetime of the gas-dust protoplanetary disk. We discuss peculiarities of the structure of planetesimals.
Makalkin A. B.
Ziglina I. N.
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