The observation of massive exoplanets at large separation ( \gtrsim 10 AU ) from their host star , like in the HR 8799 system , challenges theories of planet formation . A possible formation mechanism involves the fragmentation of massive self-gravitating discs into clumps . While the conditions for fragmentation have been extensively studied , little is known of the subsequent evolution of these giant planet embryos , in particular their expected orbital migration . Assuming a single planet has formed by fragmentation , we investigate its interaction with the gravitoturbulent disc it is embedded in . Two-dimensional hydrodynamical simulations are used with a simple prescription for the disc cooling . A steady gravitoturbulent disc is first set up , after which simulations are restarted including a planet with a range of masses approximately equal to the clump ’ s initial mass expected in fragmenting discs . Planets rapidly migrate inwards , despite the stochastic kicks due to the turbulent density fluctuations . We show that the migration timescale is essentially that of type I migration , with the planets having no time to open a gap . In discs with aspect ratio \sim 0.1 at their forming location , planets with a mass comparable to , or larger than Jupiter ’ s can migrate in as short as 10 ^ { 4 } years , that is , about 10 orbits at 100 AU . Massive planets formed at large separation from their star by gravitational instability are thus unlikely to stay in place , and should rapidly migrate towards the inner parts of protoplanetary discs , regardless of the planet mass .