Issue |
A&A
Volume 397, Number 1, January I 2003
|
|
---|---|---|
Page(s) | 275 - 284 | |
Section | Stellar atmospheres | |
DOI | https://doi.org/10.1051/0004-6361:20021512 | |
Published online | 11 December 2002 |
Mg, Ba and Eu abundances in thick disk and halo stars*
1
Department of Astronomy, Kazan State University, Kremlevskaya 18, 420008 Kazan 8, Russia
2
Institut für Astronomie und Astrophysik der Universität München, Scheinerstr. 1, 81679 München, Germany
3
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Straße 1, 85740 Garching, Germany
4
Istituto Nazionale di Astrofisica (INAF) – Osservatorio Astronomico di Torino, Via Osservatorio 20, 10025 Pino Torinese (Torino), Italy
5
Institute of Physics, Rostov State University, and Isaac Newton Institute of Chile Rostov-on-Don Branch, Stachki H. 194, 344090 Rostov-on-Don, Russia
Corresponding author: L. Mashonkina, Lyudmila.Mashonkina@ksu.ru
Received:
28
August
2002
Accepted:
7
October
2002
Our sample of cool dwarf stars from previous papers (Mashonkina &
Gehren [CITE]) is extended in this study including 15 moderately
metal-deficient stars. The samples of halo and thick disk stars have overlapping
metallicities with [Fe/H] in the region from -0.9 to -1.5, and we compare
chemical properties of these two kinematically different stellar populations
independent of their metallicity. We present barium, europium and magnesium
abundances for the new sample of stars. The results are based on NLTE line
formation obtained in differential model atmosphere analyses of high resolution
spectra observed mainly using the UVES spectrograph at the VLT of the European
Southern Observatory. We confirm the overabundance of Eu relative to Mg in halo
stars as reported in our previous papers. Eight halo stars show [Eu/Mg] values
between 0.23 and 0.41, whereas stars in the thick and thin disk display a
solar europium to magnesium ratio. The [Eu/Ba] values found in the thick disk
stars to lie between 0.35 and 0.57 suggest that during thick disk formation
evolved low-mass stars started to enrich the interstellar gas by s-nuclei of Ba,
and the s-process contribution to barium thus varies from 30% to 50%. Based on
these results, and using the chemical evolution calculations by Travaglio et al.
([CITE]), we estimate that the thick disk stellar population formed on a
timescale between 1.1 to 1.6 Gyr from the beginning of the protogalactic
collapse. In the halo stars the [Eu/Ba] values are found mostly between 0.40
and 0.67, which suggests a duration of the halo formation of about 1.5 Gyr.
For the whole sample of stars we present the even-to-odd Ba isotope ratios as
determined from hyperfine structure seen in the resonance line
. As expected, the solar ratio 82:18 (Cameron [CITE])
adjusts to observations of the
lines in the thin disk stars. In our
halo stars the even-to-odd Ba isotope ratios are close to the pure r-process
ratio 54:46 (Arlandini et al. [CITE]), and in the thick disk stars the
isotope ratio is around 65:35 (±10%). Based on these data we deduce for
thick disk stars the ratio of the
-process contribution to barium as 30:70
(±30%), in agreement with the results obtained from the [Eu/Ba] values.
Key words: line: formation / nuclear reactions, nucleosynthesis, abundances / stars: abundances / stars: late-type / Galaxy: evolution
© ESO, 2003
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