Terrestrial Planet Formation in Disks with Varying Surface Density Profiles

The “minimum-mass solar nebula” (MMSN) model estimates the surface density distribution of the protoplanetary disk by assuming the planets to have formed in situ. However, significant radial migration of the giant planets likely occurred in the Solar system, implying a distortion in the values derived by the MMSN method. The true density profiles of protoplanetary disks is therefore uncertain. Here we present results of simulations of late-stage terrestrial accretion, each starting from a disk of planetary embryos. We assume a power-law surface density profile that varies with heliocentric distance r as r−α, and vary α between 1/2 and 5/2 (α = 3/2 for the MMSN model). We find that for steeper profiles (higher values of α), the terrestrial planets (i) are more numerous, (ii) form more quickly, (iii) form closer to the star, (iv) are more massive, (v) have higher iron contents, and (vi) have lower water contents. However, the possibility of forming potentially habitable planets does not appear to vary strongly with α. Subject headings: astrobiology — planets and satellites: formation — methods: n-body simulations