In recent years several planets have been discovered at wide orbits ( > 100 AU ) around their host stars .
Theoretical studies encounter difficulties in explaining their formation and origin .
Here we propose a novel scenario for the production of planetary systems at such orbits , through the dynamical recapture of free floating planets ( FFPs ) in dispersing stellar clusters and stellar associations .
This process is a natural extension of the recently suggested scenario for the formation of wide stellar binaries .
We use N-body simulations of dispersing clusters with 10 - 1000 stars and comparable numbers of FFPs to study this process .
We find that planets are captured into wide orbits in the typical range \sim { few } \times 100 - 10 ^ { 6 } AU , and have a wide range of eccentricities ( thermal distribution ) .
Typically , 3 - 6 \times ( f _ { { FFP } } / 1 ) % of all stars capture a planetary companion with such properties ( where f _ { { FFP } } is the number of FFP per star in the birth clusters ) .
The planetary capture efficiency is comparable to that of capture-formed stellar-binaries , and shows a similar dependence on the cluster size and structure .
It is almost independent of the specific planetary mass ; planets as well as sub-stellar companions of any mass can be captured .
The capture efficiency decreases with increasing cluster size , and for a given cluster size the it increases with the host/primary mass .
We also find that more than one planet can be captured around the same host through independent consecutive captures ; similarly planets can be captured into binary systems , both in circumstellar and circumbinary orbits .
We also expect planets to be captured into pre-existing planetary ( and protoplanetary systems ) as well as into orbits around black holes and massive white dwarfs , if these formed early enough before the cluster dispersal .
In particular , stellar black holes have a high capture efficiency ( > 50 % and 5 - 10 \times ( f _ { { FFP } } / 1 ) % for capture of stars and planetary companions , respectively ) due to their large mass .
Finally , although rare , two FFPs or brown dwarfs can become bound and form a FFP-binary system with no stellar host .