Chemical Abundances and Mixing in Stars in the Milky Way and by S. Randich, L. Pasquini
By S. Randich, L. Pasquini
This lawsuits covers issues from chemical abundances within the assorted parts of the Milky method and in neighborhood team galaxies, through observational and theoretical papers on blending in stars to important bang nucleosynthesis and galaxy formation and evolution. like any volumes within the sequence ESO Astrophysics Symposia, this one offers a accomplished evaluate of the leading edge of study during this topic. it's a useful reference for either scholars and researchers.
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Extra resources for Chemical Abundances and Mixing in Stars in the Milky Way and its Satellites: Proceedings of the ESO-Arcetrie Workshop held in Castiglione della Pescaia, ... September, 2004 (ESO Astrophysics Symposia)
Only in a few O-rich AGB stars the magnesium isotopic ratios have been derived showing, however, solar ratios. (2004) attempt to derive these isotopic ratios in C-rich AGB-stars with s-element enhancements. Unfortunately, the very crowded spectral regions available for that, prevented them to derive even upper or lower limits. Therefore, the issue of the 22 Ne neutron source role still remains open from the observational point of view. 2 CNO Isotopes One of the most surprising results concerning the chemical composition of AGB stars is the fact that the overwhelming majority of the galactic C-rich AGBs show a C/O ratio only slightly exceeding the unity.
G. F. Navarro, M. R. Eke: ApJ 597, 21 (2003) C. S. L. Lambert, K. Cunha: A&A 420, 183 (2004) T. Bensby, S. Feltzing, I. Lundstr¨ om: A&A 410, 527 (2003) T. Bensby, S. Feltzing, I. Lundstr¨ om: A&A 415, 155 (2004) T. Bensby, S. Feltzing, I. B. Brook, D. K. C. Freeman: ApJ 612, 894 (2004) A. W. Truran, G. Q. E. Nissen, G. W. Zhang, T. J. A. Bernstein: AJ 124,1328 (2002) K. Fuhrmann: A&A 338, 161 (1998) K. Fuhrmann: AN 325, 3 (2004) G. G: Wyse, K. G. Gratton, E. Carretta, S. Desidera, S. Lucatello, P.
The abundance gradient: Fig. 1d). In the latter panel we have also used information coming in part from our spectroscopic work (, ), and in part from literature (, , ). While photometric and spectroscopic metallicities do reasonably agree (the most discrepant cases being NGC6253 for which the spectroscopic value is only preliminary, and 10 A. Bragaglia & M. Tosi Fig. 1. Results based on 17 OC’s: (a) Diﬀerence in magnitude between the red clump and the turn-oﬀ as a function of age; (b) and (c) age distribution with Galactocentric distance or metallicity; (d) radial distribution of metallicity (ﬁlled dots refer to photometric metallicity; when metallicity from high resolution spectroscopy is also available it is represented by asterisks and photometric metallicity by open dots).