Statistics – Computation
Scientific paper
Sep 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...262..455g&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 262, no. 2, p. 455-467.
Statistics
Computation
51
Abundance, Chemical Evolution, Computational Astrophysics, Spiral Galaxies, Astronomical Models, Galactic Mass
Scientific paper
Numerical and analytical models of the chemical evolution of the galactic disk are constructed to explore the conditions under which the observed radial abundance gradients can be explained. Constraints on the radial variations of model parameters are given. Gradients may build up sufficiently fast, if the star formation rate depends on the gas density g stronger than g1. Radial gas flows alone cannot produce any abundance gradient, but are an efficient process to amplify a pre-existing one or one generated by any other means: slow infall of primordial gas with a radially varying rate in conjunction with radial flows can produce strong negative abundance gradients. For the Galactic disk numerical computations with detailed stellar nucleosynthesis are conducted in order to reproduce the gradients observed in various nuclides, as well as to satisfy other observational constraints. Gradients of abundance ratios are shown to depend on the ratio of secondary to primary production modes. For (C-12)/(C-13) and N/O the presently available data on stellar nucleosynthesis is in agreement with the observed ratio gradients.
Goetz Martin
Koeppen Joachim
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