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