论文标题
银河系内部地区的重元素进化
Heavy element evolution in the inner regions of the Milky Way
论文作者
论文摘要
我们为内部银河系区域（$ r_ {gc} <4 $ kpc）介绍了重元素（O，Mg，Si，Ca，Mn，Mn，Ni和Fe）的丰度演变的结果。我们采用了已经测试过银河膨胀的详细化学演化模型，并将结果与Apogee数据进行了比较。我们从文献的一系列产量开始，这些产量被认为是在太阳附近重现丰度模式的最佳选择。我们发现，总的来说，预测趋势可以很好地再现数据，但在某些情况下，即使是大因素，也需要纠正预测丰度的趋势或绝对值才能达到最佳一致性。我们建议如何修改当前的恒星产量以重现数据，并根据当前对恒星核合成的知识来讨论此类校正是否合理。但是，我们还批判性地讨论了观察结果。我们的结果表明，Si，Ca，Cr和Ni是所需校正最小的要素，而对于Mg和Al中等修改是必要的。另一方面，O和K需要最大的校正来重现观察到的模式，除了氧气外，已经得出了太阳附近丰度模式的结论。对于MN，我们应用了以前的工作中已经建议的更正。 \ end {摘要}
We present results for the evolution of the abundances of heavy elements (O, Mg, Al, Si, K, Ca, Cr, Mn, Ni and Fe) in the inner Galactic regions ($R_{GC} < 4$kpc). We adopt a detailed chemical evolution model already tested for the Galactic bulge and compare the results with APOGEE data. We start with a set of yields from the literature which are considered the best to reproduce the abundance patterns in the solar vicinity. We find that in general the predicted trends nicely reproduce the data but in some cases either the trend or the absolute values of the predicted abundances need to be corrected, even by large factors, in order to reach the best agreement. We suggest how the current stellar yields should be modified to reproduce the data and we discuss whether such corrections are reasonable in the light of the current knowledge of stellar nucleosynthesis. However, we also critically discuss the observations. Our results suggest that Si, Ca, Cr and Ni are the elements for which the required corrections are the smallest, while for Mg and Al moderate modifications are necessary. On the other hand, O and K need the largest corrections to reproduce the observed patterns, a conclusion already reached for solar vicinity abundance patterns, with the exception of oxygen. For Mn we apply corrections already suggested in previous works. \end{abstract}
