  We investigate the chemical composition of the solar system's giant planets
atmospheres using a physical formation model with chemistry. The model
incorporate disk evolution, pebbles and gas accretion, type I and II migration,
simplified disk photoevaporation and solar system chemical measurements. We
track the chemical compositions of the formed giant planets and compare them to
the observed values. Two categories of models are studied: with and without
disk chemical enrichment via photoevaporation. Predictions for the Oxygen and
Nitrogen abundances, core masses, and total amount of heavy elements for the
planets are made for each case. We find that in the case without disk PE, both
Jupiter and Saturn will have a small residual core and comparable total amounts
of heavy elements in the envelopes. We predict oxygen abundances enrichments in
the same order as carbon, phosphorus and sulfur for both planets. Cometary
Nitrogen abundances does not allow to easily reproduce Jupiter's nitrogen
observations. In the case with disk PE, less core erosion is needed to
reproduce the chemical composition of the atmospheres, so both planets will end
up with possibly more massive residual cores, and higher total mass of heavy
elements. It is also significantly easier to reproduce Jupiter's Nitrogen
abundance. No single was disk was found to form both Jupiter and Saturn with
all their constraints in the case without photoevaporation. No model was able
to fit the constraints on Uranus & Neptune, hinting toward a more complicated
formation mechanism for these planets. The predictions of these models should
be compared to the upcoming Juno measurements to better understand the origins
of the solar system giant planets.
