Chemical evolution of elliptical galaxies

Details Chemical evolution of elliptical galaxies Chemical evolution of elliptical galaxies

Oct 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...185...51m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 185, no. 1-2, Oct. 1987, p. 51-60.

Astronomy and Astrophysics

Astrophysics

175

Chemical Evolution, Cosmochemistry, Elliptical Galaxies, Galactic Evolution, Nuclear Fusion, Supernova Remnants, Abundance, Binary Stars, Galactic Mass, Intergalactic Media, Red Shift, White Dwarf Stars

Scientific paper

The evolution of O-16, Mg-24, Si-28, and Fe-56 in the gas and stars of elliptical galaxies of initial mass (1-2000) x 10 to the 9th solar masses is investigated by means of numerical simulations, taking SN-powered galactic winds and the nucleosynthesis results of Woosley and Weaver (1986) into account. The theoretical basis of the models and the observational constraints are discussed in detail, and the results are presented in tables and graphs. Findings reported include (1) an Fe/galactic-mass relation significantly steeper than the relations for O, Mg, Si, and global metal content (Z); (2) a strong dependence of the time of occurence of galactic winds on the SN rate and the initial mass function; (3) type I SN rates peaking 100-300 Myr after galaxy formation; and (4) present type I SN rates in good agreement with observations.

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