The chemical evolution of spiral galaxies - M51, NGC 2403, NGC 6946 and IC 342

Details The chemical evolution of spiral galaxies - M51, NGC 2403, NGC 6946 and IC 342 The chemical evolution of spiral galaxies - M51, NGC 2403, NGC 6946 and IC 342

Dec 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985mnras.217..571t&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 217, Dec. 1, 1985, p. 571-584. CNR-supported research.

Astronomy and Astrophysics

Astronomy

40

Chemical Evolution, Galactic Evolution, Interstellar Matter, Spiral Galaxies, Abundance, Carbon Monoxide, H Ii Regions, Metallicity, Molecular Clouds, Oxygen, Stellar Evolution

Scientific paper

The chemical evolution of a number of nearby spiral galaxies is investigated by using numerical models constrained by the gas and total mass distributions presently observed in these galaxies. The oxygen abundance is computed by means of the most recent results of the stellar nucleosynthesis. The results of the models are then compared with the oxygen distributions derived from the analysis of their H II regions. A reasonably good agreement between computed and observed abundances is attained. The effect on the models of adopting different molecular hydrogen distributions resulting from the use of different CO-H2 conversion factors is discussed for all the spiral galaxies for which both neutral and molecular hydrogen distributions are available. It is found that CO distributions corrected for the metallicity gradient observed through the disks of the galaxies provide model results in better agreement with observations.

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