Other
Scientific paper
Dec 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mcdg.proc..193r&link_type=abstract
The Magellanic Clouds and Other Dwarf Galaxies, Proceedings of the Bonn/Bochum-Graduiertenkolleg Workshop, held at the Physikzen
Other
Chemical Evolution Of Dwarf Galaxies, Metal Abundance
Scientific paper
Main criteria for comparing observations of dwarf galaxies with evolutionary simulations are the metal abundances and adundance ratios, especially those for oxygen and N/O. Models of chemical evolution usually start with a high N/O ratio at low O abundance and reproduce the observed N/O-O peculiarities by the application of multiple starbursts. Their galactic winds are invoked to reduce O selectively. Our chemodynamical models of dwarf galaxies, however, demonstrate that strong evaporation of clouds in hot supernova-expelled gas leads to an almost perfect mixing of the interstellar medium and its element abundances. Hot, metal-enriched gas expands over the dwarf galaxies and condensates preferably in the outer parts. Gas clouds falling back into the inner regions therefore show almost homogeneous element abundances. First results indicate that by taking into consideration both dynamical and chemical evolution processes in a self-consistent way, we can explain the observed N/O-O values without the assumption of artificial starbursts but by using recent stellar yields which provide secondary nitrogen production also in massive stars. Here we present some features of the dynamical evolution of a simulated 10^9 M-sun dwarf irregular galaxy.
Hensler Gerhard
Rieschick Andreas
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