Volume 553, May 2013
|Number of page(s)||13|
|Section||Galactic structure, stellar clusters and populations|
|Published online||30 April 2013|
We present in Fig. A.1, the results of our inhomogenous model, with and without the “extended” site for the r-process. Thanks to the inhomogeneous model, it is possible to highlight that if we use only the “standard” r-process site (left panel), most of the stars showing a low [Ba/Fe] cannot be reproduced by our model. This problem is not clear from the results of the homogeneous model because the simple line representing the homogeneous results cannot display that a negligible amount of stars are formed by the model in this area.
[Ba/Fe] vs. [Fe/H] results; on the left the model for an r-process contribution only from the “standard” site, on the right the r-model, where both “standard” and “extended” contributions are considered. The density plot is the distribution of simulated long-living stars for our models; the density is on a log scale, normalized to the peak of the distribution (see bar over the Fig. 2 for the color scale). Superimposed, we show the abundances ratios for halo stars (data from Frebel 2010). The symbols are the same as in Fig. 3.
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© ESO, 2013
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