  The orbital elements of extreme mass ratio binaries will be modified by
interactions with surrounding circumstellar disks. For brown dwarf companions
to Solar-type stars the resulting orbital migration is sufficient to drive
short period systems to merger, creating a brown dwarf desert at small
separations. We highlight the similarities and the differences between the
migration of brown dwarfs and massive extrasolar planets, and discuss how
observations can test a migration model for the brown dwarf desert.
