Planets are formed in protoplanetary disks of gas and dust around young stars. Where and when a planet forms determines its ultimate composition. However, our ability to determine exoplanet compositions from observations is extremely limited. To truly understand what planets are made of we must instead observe the planet-forming material in the natal disk. These protoplanetary disks are dynamic objects. Material moves through the disk, experience a wide range of temperature, irradiation, and ionization conditions. Simultaneously, chemical reactions change the composition of the disk material. The full extend of chemical variation, both across a single systems evolution and between systems, in not well understood. I will lay out the tension between observational constraints on chemical timescales in disks and current protoplanetary disk models. I will then present how my research provides new insight into the evolution of protoplanetary disks by combining multi-wavelengths observations across evolutionary stages with new chemo-dynamic models. This approach provides a holistic understanding the physical and chemical conditions during planet formation.
