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We present a basic, fast, and flexible planet formation model, called SimAb(Simulating Abundances), to form giant planets and study their primaryatmospheric composition soon after their formation. In SimAb we introduceparameters to simplify the assumptions about the complex physics involved inthe formation of a planet. This approach allows us to trace and understand theinfluence of complex physical processes on the formed planets. We focus on theC/O ratio and the metallicity of the planetary atmosphere as an indicator oftheir compositions. We show that the initial protoplanet core mass does notinfluence the final composition of the planetary atmosphere in the context ofour model. The initial orbital distance affects the C/O ratio due to thedifferent C/O ratios in the gas phase and the solid phase at different orbitaldistances. Additionally, the initial orbital distance together with the amountof accreted planetesimals cause the planet to have sub-solar or super-solarmetallicity. Furthermore, the C/O ratio is affected by the dust grain fractionand the planetesimal fraction. Planets that accrete most of their heavyelements through dust grains will have a C/O ratio close to the solar C/Oratio, while planets that accrete most of their heavy elements from theplanetesimals in the disk will end up with a C/O ratio closer to the C/O ratioin the solid phase of the disk. By using the C/O ratio and metallicity togetherwe can put a lower and upper boundary on the initial orbital distance wheresuper-solar metallicity planets are formed. We show that planetesimals are themain source for reaching super-solar metallicity planets. On the other hand,planets that mainly accrete dust grains will show a more solar composition.Super-solar metallicity planets that initiate their formation farther than theCO ice line have a C/O ratio closer to the solar value.

SimAb: A simple, fast and flexible model to assess the effects of planet formation on the atmospheric composition of gas giants