Chemical evolution models for spiral disks: the Milky Way, M 31, and M 33

M 33 and the Milky Way : Similarities and Differences Rosemary

The large galaxies in the Local Group, while all disk galaxies, have diverse stellar populations. A better understanding of these differences, and a physical understanding of the causes, requires more detailed study of the older populations. This presents a significant challenge to GAIA but the scientific returns are also significant.

The Chemical Evolution of the Milky Way

Second - parameter Globular Clusters in the Milky Way and in M 33 as Tracers of Mass Loss from M 31 in the Early Epoch ?

I suggest that the bulk of the ”young”, second-parameter globular clusters (SPGCs) observed in the outer halo of our Galaxy and recently found in other massive spiral of the Local Group (LG), M33, may have originated due to mass outflow from M31 and subsequent accretion of gas on the Galaxy and M33 in the early epoch. 1. Problem and Main Questions There are contradictory conclusions about the d...

Meteorites and the Chemical Evolution of the Milky Way

1100. Lunar and Planetary Institute, Houston (CD-ROM). Dearborn D. S. P. (1992) Diagnostics of stellar evolution: The oxygen isotopes. Phys. Rept., 210, 367–382. Dopita M. A. and Ryder S. D. (1994) On the law of star formation in disk galaxies. Astrophys. J., 430, 163–178. Edvardsson B., Anderson J., Gustaffson B., Lambert D. L., NissenP. E., and Tomkin J. (1993) The chemical evolution ...

Chemical evolution and abundance gradients in the Milky Way

We extend our model of chemical evolution that successfully account for the main observables in the solar neighborhood (Alibés, Labay & Canal 2001) to the whole Milky Way halo and disk. We assume an inside–out scenario for the assembling of the Galaxy through the infall of external material. Two different compositions of the infalling material have been considered: primordial and slightly metal...