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Embedded in the gaseous protoplanetary disk, Jupiter and Saturn naturallybecome trapped in 3:2 resonance and migrate outward. This serves as the basisof the Grand Tack model. However, previous hydrodynamical simulations wererestricted to isothermal disks, with moderate aspect ratio and viscosity. Herewe simulate the orbital evolution of the gas giants in disks with viscousheating and radiative cooling. We find that Jupiter and Saturn migrate outwardin 3:2 resonance in modest-mass ($M_{disk} \approx M_{MMSN}$, where MMSN is the"minimum-mass solar nebula") disks with viscous stress parameter $\alpha$between $10^{-3}$ and $10^{-2} $. In disks with relatively low-mass ($M_{disk}\lesssim M_{MMSN}$) , Jupiter and Saturn get captured in 2:1 resonance and caneven migrate outward in low-viscosity disks ($\alpha \le 10^{-4}$). Such diskshave a very small aspect ratio ($h\sim 0.02-0.03$) that favors outwardmigration after capture in 2:1 resonance, as confirmed by isothermal runs whichresulted in a similar outcome for $h \sim 0.02$ and $\alpha \le 10^{-4}$. Wealso performed N-body runs of the outer Solar System starting from the resultsof our hydrodynamical simulations and including 2-3 ice giants. After dispersalof the gaseous disk, a Nice model instability starting with Jupiter and Saturnin 2:1 resonance results in good Solar Systems analogs. We conclude that in acold Solar Nebula, the 2:1 resonance between Jupiter and Saturn can lead tooutward migration of the system, and this may represent an alternative scenariofor the evolution of the Solar System.

Outward migration of Jupiter and Saturn in 3:2 or 2:1 resonance in radiative disks: implications for the Grand Tack and Nice models