Abstract
Several relevant properties of evolving stellar populations are discussed from a theoretical viewpoint. These include the absolute and specific evolutionary flux of a stellar population, the relative contributions of stars in the various evolutionary stages, the bolometric evolution, and the total and specific rates of mass return. We then introduce the concept of phase transition in the stellar content of a population, an event which is produced by the first appearance of stars with either C-O or He degenerate cores. The spectral energy distribution of a population is then predicted to suffer a (major) change at each of these phase transitions. Some uncertainties in both current stellar and population evolutionary models, and in population synthesis techniques are then briefly discussed, and the need is emphasized for appropriate checks and calibrations using template stellar populations. Magellanic Cloud Clusters offer the best tool for these purposes, and we then discuss in some detail current problems in dating MC clusters, as well as the origin of the blue to red transition in these clusters and its possible connection with the mentioned phase transitions. Finally, as examples of how some of these concepts could be applied to real galaxies, we discuss the possible occurrence and detection of population phase transition in high redshift elliptical galaxies, as well as the origin of the ultraviolet light of ellipticals and its predicted behaviour with look back time.
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Renzini, A., Buzzoni, A. (1986). Global Properties of Stellar Populations and the Spectral Evolution of Galaxies. In: Chiosi, C., Renzini, A. (eds) Spectral Evolution of Galaxies. Astrophysics and Space Science Library, vol 122. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-4598-2_19
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DOI: https://doi.org/10.1007/978-94-009-4598-2_19
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