I will review the basic methods to build chemical evolution models for the Milky Way as well as their uncertainties and strengths. All the main ingredients (initial conditions, birthrate function, stellar yields, gas flows) will be discussed. Then, the basic equations of galactic chemical evolution will be introduced. The importance of considering stellar lifetimes and supernovae of all types II, Ia, Ib/c) will be highlighted. Then I will compare different model predictions with observables, in particular the [X/Fe] vs. [X/H] diagrams as well as abundance, gas and star formation gradients along the disk.

I will show that from this comparison one can infer constraints on stellar nucleosynthesis and on the typical timescales and mechanisms for the formation of the various components of the Milky Way (Halo, Disk and Bulge). A comparison between the stellar abundances of the Milky Way and those of the dwarf spheroidals of the Local Group will be presented in order to check if these galaxies have been the building blocks of our Galaxy. Finally, I will show that the above described galactic astroarchaelogy is also very useful to compare with the predictions of models based on cosmological simulations.