We present a chemical evolution model of our galaxy to fit the O/H gradients of H II regions. This model produces an excellent fit to the observational stellar constraints (B-stars, Cepheids, F-G dwarfs, red giant stars and the Sun). The model reproduces the flattening observed in the 3–6 kpc galactocentric range; this flattening is attained with an inside-out star formation quenching in the inner disk starting ∼ 9 Gyr ago.
Enviado por carigi@astro.unam.mx, 2019 Sep