We present results from 42 simulations of late stage planetary accretion , focusing on the delivery of volatiles ( primarily water ) to the terrestrial planets .
Our simulations include both planetary “ embryos ” ( defined as Moon to Mars sized protoplanets ) and planetesimals , assuming that the embryos formed via oligarchic growth .
We investigate volatile delivery as a function of Jupiter ’ s mass , position and eccentricity , the position of the snow line , and the density ( in solids ) of the solar nebula .

In all simulations , we form 1-4 terrestrial planets inside 2 AU , which vary in mass and volatile content .
In 42 simulations we have formed 43 planets between 0.8 and 1.5 AU , including 11 “ habitable ” planets between 0.9 and 1.1 AU .
These planets range from dry worlds to “ water worlds ” with 100+ oceans of water ( 1 ocean = 1.5 \times 10 ^ { 24 } g ) , and vary in mass between 0.23 { M _ { \oplus } } and 3.85 { M _ { \oplus } } .

There is a good deal of stochastic noise in these simulations , but the most important parameter is the planetesimal mass we choose , which reflects the surface density in solids past the snow line .
A high density in this region results in the formation of a smaller number of terrestrial planets with larger masses and higher water content , as compared with planets which form in systems with lower densities .

We find that an eccentric Jupiter produces drier terrestrial planets with higher eccentricities than a circular one .
In cases with Jupiter at 7 AU , we form what we call “ super embryos , ” 1-2 { M _ { \oplus } } protoplanets which can serve as the accretion seeds for 2+ { M _ { \oplus } } planets with large water contents .