The metallicity distribution of G dwarfs in the solar neighbourhood and the chemical evolution of the Galaxy

Based on a new metallicity distribution for G dwarfs within 25 pc of the sun this paper discusses in detail four galactic chemical evolution models in an inhomogeneous interstellar medium. It is shown that both the so-called simple model and the collapse model deviate greatly from the observations, while the two models labelled PIE (Prompt Initial Enrichment) and PPY (Proportional Yield) not only give much better fit, but also alleviate the so-called G-dwarf problem. The indications are that the outer halo has little influence on the chemical evolution near the Sun.