  We study a Jupiter-mass planet formation for the first time in radiative
magneto-hydrodynamics (MHD) simulations and compare it with pure hydrodynamical
simulations, as well as to different isothermal configurations. We found that
the meridional circulation is the same in every setup. The planetary spiral
wakes drive a vertical stirring inside the protoplanetary disc and the
encounter with these shock fronts also helps in delivering gas vertically onto
the Hill-sphere. The accretion dynamics are unchanged: the planet accretes
vertically, and there is outflow in the midplane regions inside the
Hill-sphere. We determined the effective $\alpha$-viscosity generated in the
disc by the various angular momentum loss mechanisms, which showed that
magnetic fields produce high turbulence in the ideal MHD limit, that grows from
$\alpha \sim 10^{-2.5}$ up to $\sim 10^{-1.5}$ after the planet spirals
develop. In the HD simulations, the planetary spirals contribute to $\alpha
\sim 10^{-3}$, making this a very important angular momentum transport
mechanism. Due to the various $\alpha$ values in the different setups, the gap
opening is different in each case. In the radiative MHD setups, the high
turbulent viscosity prevents gap opening, leading to a higher Hill mass, and no
clear dust trapping regions. While the Hill accretion rate is $10^{-6}
\rm{M_{Jup}/yr}$ in all setups, the accretion variability is orders of
magnitude higher in radiative runs than in isothermal ones. Finally, with
higher-resolution runs, the magneto-rotational instability started to be
resolved, changing the effective viscosity and increasing the heating in the
disc.
