  For the very first time we present 3D simulations of planets embedded in
stellar irradiated discs. It is well known that thermal effects could reverse
the direction of planetary migration from inwards to outwards, potentially
saving planets in the inner, optically thick parts of the protoplanetary disc.
When considering stellar irradiation in addition to viscous friction as a
source of heating, the outer disc changes from a shadowed to a flared
structure. Using a suited analytical formula it has been shown that in the
flared part of the disc the migration is inwards; planets can migrate outwards
only in shadowed regions of the disc, { because the radial gradient of entropy
is stronger there}. In order to confirm this result numerically, we have
computed the total torque acting on planets held on fixed orbits embedded in
stellar irradiated 3D discs using the hydrodynamical code FARGOCA. We find
qualitatively good agreement between the total torque obtained with numerical
simulations and the one predicted by the analytical formula. For large masses
(>20 Earth masses) we find quantitative agreement, and we obtain outwards
migration regions for planets up to 60 Earth masses in the early stages of
accretional discs. We find nevertheless that the agreement with the analytic
formula is quite fortuitous because the formula underestimates the size of the
horseshoe region; this error is compensated by imperfect estimates of other
terms, most likely the cooling rate and saturation.
