Astronomy and Astrophysics – Astrophysics
Scientific paper
2000-07-12
Astronomy and Astrophysics
Astrophysics
18 pages, 10 figures, 1 Table, Astronomy and Astrophysics, accepted for publication
Scientific paper
Based on a simple, but fairly successful, model of the chemical evolution of the Milky Way disk, we study the evolution of the abundances of the elements He, C, N, O, Ne, Mg, Al, Si, S, Ar and Fe. We use metallicity dependent yields for massive stars with and without mass loss. We find that most observed abundance profiles are correctly reproduced by massive star yields, but C and N require supplementary sources. We argue that massive, mass losing stars can totally account for the abundance profile of C, while intermediate mass stars are the main source of N; in both cases, some conflict with corresponding data on extragalactic HII regions arises, at least if current observations in the Galaxy are taken at face value. The observed behaviour of Al is marginally compatible with current massive star yields, which probably overestimate the ``odd-even'' effect. We also find that the adopted ``inside-out'' formation scheme for the Milky Way disk produce abundance profiles steeper in the past. The corresponding abundance scatter is smaller in the inner disk than in the outer regions for a given interval of Galactic age.
Boissier Samuel
Hou Lu-Jing
Prantzos Nikos
No associations
LandOfFree
Abundance gradients and their evolution in the Milky Way disk does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Abundance gradients and their evolution in the Milky Way disk, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Abundance gradients and their evolution in the Milky Way disk will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-279179