Chemical and luminosity evolution, and counts of galaxies in a merger model

Details Chemical and luminosity evolution, and counts of galaxies in a merger model Chemical and luminosity evolution, and counts of galaxies in a merger model

Apr 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...407..510c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 407, no. 2, p. 510-518.

Statistics

Computation

6

Astronomical Models, Chemical Evolution, Galactic Evolution, Interacting Galaxies, Luminosity, Abundance, Mathematical Models, Metallicity, Star Formation, Supernovae

Scientific paper

A merger model is applied to the chemical and luminosity evolution of galaxies. Two aspects are focused on. The first is the problem of abundance ratios as a function of metallicity. The second is related to the luminosity evolution of galaxies. In relation to the former, we calculate the evolution of several chemical elements exploring a broad space of possible star formation rates, including those derived using phenomenological arguments from a multiple merger galaxy formation scenario. We are able to reproduce the observed plateau in the ratio of the abundances of oxygen to iron versus metallicity as a direct consequence of one of the merging SFR used; we have utilized a standard Type II supernovae nucleosynthesis scenario coupled with a reasonable binary model for Type Ia supernovae and its consequent nucleosynthetic yields. Following the consequent luminosity effects in a straightforward way enables the estimation of the evolution of bolometric luminosity. We have used our recently developed code for photometric evolution of galaxies to make a preliminary computation of the number-magnitude relationship, assuming a standard picture of galaxy evolution, in the B and K bands.

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