  As planets grow the exchange of angular momentum with the gaseous component
of the protoplanetary disc produces a net torque resulting in a variation of
the semi-major axis of the planet. For low-mass planets not able to open a gap
in the gaseous disc this regime is known as type I migration. Pioneer works
studied this mechanism in isothermal discs finding fast inward type I migration
rates that were unable to reproduce the observed properties of extrasolar
planets. In the last years, several improvements have been made in order to
extend the study of type I migration rates to non-isothermal discs. Moreover,
it was recently shown that if the planet's luminosity due to solid accretion is
taken into account, inward migration could be slowed down and even reversed. In
this work, we study the planet formation process incorporating, and comparing,
updated type I migration rates for non-isothermal discs and the role of
planet's luminosity over such rates. We find that the latter can have important
effects on planetary evolution, producing a significant outward migration for
the growing planets.
