The Signature of the Ice Line and Modest Type I Migration in the Observed Exoplanet Mass-Semimajor Axis Distribution

Existing exoplanet radial velocity surveys are complete in the planetary masssemimajor axis (Mp − a) plane over the range 0.1 AU < a < 2.0 AU where Mp & 100 M⊕. We marginalize over mass in this complete domain of parameter space and demonstrate that the observed a distribution is inconsistent with models of planet formation that use the full Type I migration rate derived from a linear theory and that do not include the effect of the ice line on the disk surface density profile. However, the efficiency of Type I migration can be suppressed by both nonlinear feedback and the barriers introduced by local maxima in the disk pressure distribution, and we confirm that the synthesized Mp − a distribution is compatible with the observed data if we account for both retention of protoplanetary embryos near the ice line and an order-of-magnitude reduction in the efficiency of Type I migration. The validity of these assumption can be checked because they also predict a population of short-period rocky planets with a range of masses comparable to that of the Earth as well as a “desert” in the Mp − a distribution centered around Mp ∼ 30− 50 M⊕ and a < 1 AU. We show that the expected “desert” in the Mp − a plane will be discernible by a radial velocity survey with 1 m s precision and n ∼ 700 radial velocity observations of program stars. Subject headings: planetary systems — planetary systems: formation — planetary systems: protoplanetary disks NSF Graduate Research Fellow Kavli Institute of Astronomy and Astrophysics, Peking University, Beijing, China