Lee Hartmann's Accretion Processes in Star Formation, 2nd Edition PDF

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Extra resources for Accretion Processes in Star Formation, 2nd Edition (Cambridge Astrophysics)

Sample text

6 Sheets and filaments 37 where is the surface density and E is the second complete elliptic integral. 31) where K is the first complete elliptic integral. The acceleration goes to infinity at d = R, which would not occur in a sheet with finite thickness; thus we restrict use of this equation to regions considerably more than a sheet thickness from the edge. 9 shows the acceleration in units of 4G as a function of r/R. The steep increase of inward acceleration as r → R implies that the sheet, initially at rest, will immediately proceed to collapse, with material piling up most rapidly at the outer edge (limited by gas pressure gradients which are ignored in the calculation).

The above picture of collapse and disk evolution then needs to be modified to account for more complex disk structure, such as truncation of the disks surrounding individual (proto)stars. The formation of planets is thought to occur near the end of disk evolution. The most likely mechanism for initiating planet formation is the agglomeration of dust particles in the disk. Small dust is expected to eventually settle toward the disk midplane and accumulate into larger bodies. Although small (micron-sized) dust particles are likely to stick together 20 Overview quite effectively, it is not clear that collisions can account for growth up to km-sized bodies, at which point the gravity of the bodies can take over in enhancing accretional growth.

Small dust is expected to eventually settle toward the disk midplane and accumulate into larger bodies. Although small (micron-sized) dust particles are likely to stick together 20 Overview quite effectively, it is not clear that collisions can account for growth up to km-sized bodies, at which point the gravity of the bodies can take over in enhancing accretional growth. The timescales for planetary growth are uncertain, and are likely to vary substantially even among stars of the same mass; most probably they lie in the range of a few to 10 Myr, corresponding to the timescales for the disappearance of extensive dusty disks.

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