Evolution of spiral galaxies. I - Halo-disk connection for the evolution of the solar neighborhood

Details Evolution of spiral galaxies. I - Halo-disk connection for the evolution of the solar neighborhood Evolution of spiral galaxies. I - Halo-disk connection for the evolution of the solar neighborhood

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...387..138f&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 387, March 1, 1992, p. 138-151. Research supported by MURST.

Astronomy and Astrophysics

Astrophysics

110

Galactic Evolution, Galactic Structure, Halos, Solar Neighborhood, Spiral Galaxies, Chemical Evolution, Dwarf Stars, G Stars, Metallicity, Nuclear Astrophysics, Star Formation Rate

Scientific paper

A complex model is presented for calculating the evolution of galaxies, with particular attention given to the chemical evolution of the Milky Way. The solar neighborhood is subdivided into halo and disk regions and their individual but interconnected evolution is computed in detail. The evolution of the abundances of 15 chemical species is predicted for both the halo and the disk. A new initial mass function, constant in space and time, is adopted. Cloud-cloud collisions and stimulated processes are considered as the main causes for star formation of the disk. It is shown that the majority of observational constraints for the solar neighborhood are reproduced by the model. The evolution of the relative abundances as functions of iron abundance is predicted for halo and disk stars. Considering the contemporaneous evolution of two coupled zones, an overlap of halo and disk stars is found in the metallicity range -1.6 to -1.0. Good agreement is obtained for current supernova rates, the star formation rate, and remnant, gas, and cloud masses when compared with the available data.

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