A Simple Disk Model For the Chemical Evolution of Our Galaxy

Details A Simple Disk Model For the Chemical Evolution of Our Galaxy A Simple Disk Model For the Chemical Evolution of Our Galaxy

Dec 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981jkas...14...55l&link_type=abstract

Journal of the Korean Astronomical Society, vol. 14, no. 2, p. 55-71

Astronomy and Astrophysics

Astronomy

15

Scientific paper

On the basis of observational constraints, particularly the relationship between metal abundance and cumulative stellar mass, a simple two-zone disk-halo model for the chemical evolution of our Galaxy was investigated, assuming different chemical processes in the disk and the infall rates of the halo gas defined by the halo evolution. The main results of the present model calculations are: (i) The halo formation requires more than 80% of the initial galactic mass and it takes a period of 2-3x10^9 yrs. (ii) The halo evolution is divided into two phases, a fast collapse (t=2-3x10^8 yrs) during which period most of the halo stars (~95%) are formed and a later slow collapse phase which is characterized by the chemical enrichment due to the inflow of external matter to the halo. (iii) The disk evolution is also divided into two phases, an active disk formation phase with a time-dependent initial mass function (IMF) up to t=6x10^9 yrs and a later steady slow formation phase with a constant IMF. It is rapidly increased to ~1/3 of the present value but the total stellar mass only to ~10% of the present value, finally reaching about 80% of the present values toward the end of the active formatin phase.

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