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Chemo-Dynamical Models and the Star Formation History of Galaxies

Published online by Cambridge University Press:  25 May 2016

M. Samland  and
G. Hensler
M. Samland
Affiliation:
Institut für Astronomie und Astrophysik, Universität Kiel, D-24098 Kiel, Germany
G. Hensler
Affiliation:
Institut für Astronomie und Astrophysik, Universität Kiel, D-24098 Kiel, Germany

Extract

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Sandage (1986) showed what the star formation rate (SFR) of galaxies of different Hubble type might look like. His curves are based on the study of Gallagher et al. (1984), who determined the SFR at three different epochs of galactic evolution. Sandage's figure establishes a connection of SFR and Hubble type but, as was already mentioned by Sandage, it “contains no physics”. In order to explore the background of this connection, however, it is necessary either to improve the observations or to model the evolution of galaxies self-consistently. However, the results of modelling the SFR are not reliable, if simplified models are used, which only describe some structural properties of galaxies. It is necessary to apply self-consistent models which take into consideration all relevant interaction processes between the gaseous and stellar components of a galaxy. Such models can be checked by comparison with observations like density and abundance distributions, star-gas content, velocities, velocity dispersions, mass-luminosity relations and age distributions of stars. A detailed model will show, whether the initial conditions, the feedback mechanisms during the evolution or the environment determine the evolution of a galaxy.

Type
Spiral Galaxies
Information
Symposium - International Astronomical Union , Volume 171: New Light on Galaxy Evolution , 1996 , pp. 23 - 27
Copyright
Copyright © Kluwer 1996 

References

Condon, J.J., Helou, G., Sanders, D.B., Soifer, B.T., 1990, ApJS 73, 359 Google Scholar
Dressier, A., 1979, ApJ 231, 659 Google Scholar
Gallagher, J.S., Hunter, D.A., Tutukov, A.V., 1984, ApJ 284, 544 Google Scholar
Gott, J.R., Thuan, T.X., 1976, ApJ 204, 649 Google Scholar
Hunter, D.A., Gallagher, J.S., 1986, PASP 98, 5 Google Scholar
Miyamoto, M., Satoh, C., Ohashi, M., 1980, Astrophys. Space Sci. 67, 147 Google Scholar
Roberts, M.S., Haynes, M.P., 1994, ARAA 32, 115 Google Scholar
Samland, M., 1994, Dissertation, University of Kiel, Germany Google Scholar
Samland, M., Hensler, G., 1995, IAU-Symp. 169, in press Google Scholar
Samland, M., Hensler, G., Theis, C., 1995, ApJ submitted Google Scholar
Sandage, A., Freeman, K., Stokes, N., 1970, ApJ 160, 831 Google Scholar
Sandage, A., 1986, A&A 161, 89 Google Scholar
Sofue, Y., Habe, A., 1992, PASJ 44, 325 Google Scholar
Thronson, H.A.J., Telesco, C.M., 1986, ApJ 311, 98 Google Scholar
Tully, R.B., Mould, J.R., Aaronson, M., 1982, ApJ 257, 527 Google Scholar
Tully, R.B., 1988, Nearby Galaxies Catalog, Cambridge University Press Google Scholar