Chemical Abundances and Mixing in Stars in the Milky Way and by E.D. Friel (auth.), Sofia Randich, Luca Pasquini (eds.)

By E.D. Friel (auth.), Sofia Randich, Luca Pasquini (eds.)

The box of chemical abundances and inner blending of components in stars has made huge development within the final decade. either a wealth of latest observational info and within the final years additionally the inauguration of latest theoretical roads were the stimulus for this ESO Workshop held in Castiglione della Pescaia, Italy, 13-17 September 2004.

The lawsuits disguise issues from chemical abundances within the diverse elements of the Milky means and in neighborhood staff galaxies, through observational and theoretical papers on blending in stars to special bang nucleosynthesis and galaxy formation and evolution.

As all volumes during this sequence of ESO Astrophysics Symposia this one offers a accomplished state of the art evaluate of the leading edge of analysis in its sector. it really is therefore a useful reference for either scholars focusing on the sector and researchers alike.

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Extra resources for Chemical Abundances and Mixing in Stars in the Milky Way and its Satellites: Proceedings of the ESO Workshop held in Castiglione della Pescaia, Italy, 13–17 September, 2004

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It would be especially crucial to establish if there is an age-metallicity relation in the thick disk or not as in that case the thick disk could not have formed in that way (since the models indicate that the formation time-scale for the stars in the thick disk would be very short, see [7]). Thick disks are common in other galaxies, especially in merger environments, hence perhaps we should prefer the merger scenario for the Milky Way? References 1. 2. 3. 4. 5. 6. 7. 8. 9. 10. 11. 12. 13. 14. 15.

5 (upper right) of PMS04, where N/O is plotted vs O/H. 9 (in usual units) (Grevesse & Anders, 1989; Grevesse & Sauval 1998). , 2004; Melendez, 2004, ApJ in press), the theoretical predictions would move in that diagram to the left, going closer to the observations. We favour this latter possibility, even if the line fluxes on which this lower solar oxygen abundance is based are extremely small and the abundances from the single lines depend in some cases on details of the photosphere modelling. We prefer the latter, because with the first possibility one does not see why all PNe, from those originated from more massive progenitors to those coming from about solar mass stars, should have started with an original oxygen abundance quite less than the solar one, as it’s outstandingly evident in the mentioned Fig.

Tosi, L. Greggio, G. Marconi, P. Focardi: AJ 102, 951 (1991) 3. M. Tosi, L. Di Fabrizio, A. A. Carusillo, G. Marconi: MNRAS 354, 225 (2004) 4. S. Kalirai, M. Tosi: MNRAS 351, 649 (2004) 5. A. : AJ 121, 327 (2001) 6. E. Carretta, A. G. Gratton, M. Tosi: A&A 422, 951 (2004) 7. G. Gratton, G. Contarini: A&A 283, 911 (1994) 8. V. Hill, L. Pasquini: A&A 348, L21 (1999) 9. G. Carraro, F. Bresolin, S. Villanova, F. Matteucci, F. Patat, M. Romaniello: AJ, 128, 1676 (2004) Chemical Abundances and Mixing in Red Clump Stars of the Galaxy G.

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