Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991jkas...24...25l&link_type=abstract
Journal of the Korean Astronomical Society, vol. 24, no. 1, p. 25-53
Astronomy and Astrophysics
Astronomy
3
Scientific paper
The evolution of the Galaxy is examined by the halo-disk model, using the time-dependent bimodal IMF and constraints such as cumulative metallicity distribution, differential metallicity distribution and PDMF of main sequence stars. The time scale of the Galactic halo formation is about 3 Gyr during which the most of halo stars and metal abundance are formed and ~ 95% of the initial halo mass falls to the disk. The G-dwarf problem could be explained by the time-dependent bimodal IMF which is suppressed for low mass stars at the early phase(t < 1 Gyr) of the disk evolution. However, the importance of this problem is much weakened by the Pagel's differential metallicity distribution which leads to less initial metal enrichment and many long-lived metal-poor stars with Z < 1/3 Zo. The observational distribution of abundance rations of C, N, O elements with respect to [Fe/H] could be reproduced by the halo-disk model, including the contribution of iron product by SN Is of intermediate mass stars. The initial enrichment of elements in the disk could be explained by the halo-disk model, resulting in the slight decrease and then the increase in the slopes of the [N/Fe]- and [C/Fe]-distributions with increasing [Fe/H] in the range of [Fe/H] < -1.
Ann Hong Bae
Kang Yong Hee
Lee See-Woo
Park Byeong-Gon
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