| Budget Amount *help |
¥4,550,000 (Direct Cost: ¥3,500,000、Indirect Cost: ¥1,050,000)
Fiscal Year 2011: ¥1,300,000 (Direct Cost: ¥1,000,000、Indirect Cost: ¥300,000)
Fiscal Year 2010: ¥1,300,000 (Direct Cost: ¥1,000,000、Indirect Cost: ¥300,000)
Fiscal Year 2009: ¥1,950,000 (Direct Cost: ¥1,500,000、Indirect Cost: ¥450,000)
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| Research Abstract |
Planetary systems are formed in protoplanetary disks, disk-like nebulae rotating around protostars. Dust grains in the disk are thought to grow through mutual collision to form solid planetesimals with radii greater than a few km. However, the growth process from dust to planetesimals is controversial for more than 30 years. This work investigates dust behavior in non-axisymmetric flows(vortices) derived from(magneto-) hydrodynamic instabilities in the protoplanetary disks. The semianalytic formula of dust surface density distribution is obtained. Dust is found to be concentrated around the center of an anticyclonic vortex whose age is long enough. The density of dust near the center of the vortex is large enough for dust grains to settle down to the midplane of the disk and planetsimals will be formed. This kind of planetesimal formation makes large difference in the following planetary accretion process, such as smaller number of planetesimals with radii less than 100 km.
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