The 41/2 Steps of the Core Accretion Model of Giant Planet Formation
Step 0.5: Once the the disk forms the dust settles to a the mid-plane.
Step I: Planetesimal Formation. ......
- Johansen, Henning and Klahr (2006) might have solved this long-standing problem.
- Particles settle in turbulence eddies
gravitational instabilities.
- Standard models puts the first planetesimals at 1-10km.
- This models says that the first planetesimals could be >100km.
Step II: Big guys grow faster than small guys Runaway Growth.
.............. (Greenberg et al. 1978; Wetherill & Stewart ) 
-
..............
- And since
.
- As long as
is not affected by big guys.
- Breaks down when mass is ~1025g in a Minimum Mass Solar Nebula. (Ida & Makino)
360o
Azimuth
0o
Z
