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A new model for the formation of Jovian planets is proposed. We considerplanets forming at large distances from a protostar (>100 AU) through directfragmentation of a gas cloud, by the same formation mechanism as wide stellarand brown dwarf binaries. We model the gravitational evolution of a system ofthese distant planets and a second population formed in a disk closer to thestar. We compute the typical closest approach of these planets to the star(i.e., smallest pericenter) over the course of their evolution. When theplanets reach a pericenter within a gaseous disk surroundig the star, dynamicalfriction from this disk slows down the planet at each plunge, causing its orbitto be gradually circularized and made coplanar with the disk. After the diskdissipates, a large fraction of these planets may be left at orbits smallenough to be detected in present radial velocity surveys. A brief analyticderivation of the rate of orbital energy dissipation during these diskcrossings is presented. Observational tests of this model are discussed.

Protostellar Cloud Fragmentation and Inward Migration by Disk Capture as the Origin of Massive Exoplanets