Numerical simulation of the galactic chemical evolution: The revised solar abundance

Abstract

AbstractWe have developed a numerical code for galactic chemical evolution (GCE) of all the stable isotopes from hydrogen to gallium in accordance with the recently revised bulk solar photosphere abundances (Asplund et al. 2009) and the earlier deduced abundances (Anders and Grevesse 1989), herein referred as the pre‐revised abundances. In contrast to solving the classical set of GCE equations, we have numerically simulated the evolution of the galaxy in the solar neighborhood in terms of evolution of the interstellar medium and numerous generations of stars. The evolution of the galaxy was simulated by adopting a two‐stage accretion process. Numerous generations of stars were formed from the interstellar medium according to the adopted star formation rates and the stellar initial mass function (IMF). The simulated stars were evolved and their stellar nucleosynthetic contributions toward the inventories of the stable nuclides to the galaxy were accessed. Assessments were made regarding the type Ia, Ib/c, and II supernovae rates and the stellar remnants, e.g., white‐dwarfs, neutron stars, and black holes. We have computed the age–metallicity relation and the solar abundances of the stable isotopes. A wide range of simulations were performed by parameterizing the choice of the accretion rate of the galaxy, the stellar initial mass function, the stellar evolution, and nucleosynthetic prescription to study their influence on galactic chemical evolution. The reduction in the observed solar metallicity results in significantly reduced supernova rate history of the galaxy, and a better match to the observed elemental evolutionary trend.