We present a statistical study of the post-formation migration of giant planets in a range of initial disk conditions .
For given initial conditions we model the evolution of giant planet orbits under the influence of disk , stellar , and mass loss torques .
We determine the mass and semi-major axis distribution of surviving planets after disk dissipation , for various disk masses , lifetimes , viscosities , and initial planet masses .
The majority of planets migrate too fast and are destroyed via mass transfer onto the central star .
Most surviving planets have relatively large orbital semi-major axes of several AU or larger .
We conclude that the extrasolar planets observed to date , particularly those with small semi-major axes , represent only a small fraction ( \sim 25 % to 33 % ) of a larger cohort of giant planets around solar-type stars , and many undetected giant planets must exist at large ( > 1-2 AU ) distances from their parent stars .
As sensitivity and completion of the observed sample increases with time , this distant majority population of giant planets should be revealed .
We find that the current distribution of extrasolar giant planet masses implies that high mass ( more than 1-2 Jupiter masses ) giant planet formation must be relatively rare .
Finally , our simulations imply that the efficiency of giant planet formation must be high : at least 10 % and perhaps as many as 80 % of solar-type stars possess giant planets during their pre-main sequence phase .
These predictions , including those for pre-main sequence stars , are testable with the next generation of ground- and space-based planet detection techniques .