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Chemical and Dynamical History of the Milky Way

Published online by Cambridge University Press:  25 May 2016

I.F. Bikmaev ,
L.I. Mashonkina ,
N.A. Sakhibullin ,
V.V. Shimanskij  and
N. Shimanskaya
I.F. Bikmaev
Affiliation:
Special Astrophysical Observatory, Nizhnij Arkhyz, Karachai-Circassian Republic, Russia, 357147
L.I. Mashonkina
Affiliation:
Department of Astronomy, Kazan State University, Lenin Str., 18, Kazan, Russia, 420008
N.A. Sakhibullin
Affiliation:
Department of Astronomy, Kazan State University, Lenin Str., 18, Kazan, Russia, 420008
V.V. Shimanskij
Affiliation:
Department of Astronomy, Kazan State University, Lenin Str., 18, Kazan, Russia, 420008
N. Shimanskaya
Affiliation:
Department of Astronomy, Kazan State University, Lenin Str., 18, Kazan, Russia, 420008

Extract

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F-G dwarf stars of different metallicity are used as tracers of chemical and dynamical history of the Galaxy. Observed ratios of element abundances “[X/Fe] versus [Fe/H]” (where “X” is a some of chemical element) are compared with theoretical ones and allow us to make the choice between models (or parameters of theoretical models) of the Galaxy chemical evolution, nucleosynthesis and processes of star formation. Our experience has shown (Bikmaev, 1991, 1994a,b; Bikmaev et al., 1990) that in some cases classical approaches in abundance determination are affected by methodical uncertainties and the spread in [X/Fe] ratios may be large even if high quality spectra used.

Type
Chapter 5: How Did the Milky Way Form?
Information
Symposium - International Astronomical Union , Volume 169: Unsolved Problems of the Milky Way , 1996 , pp. 389 - 394
Copyright
Copyright © Kluwer 1996 

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