Context: The chemical composition of stars is intimately linked to the Galaxy formation and evolution. Aims: We aim to trace the chemical evolution of the Galactic disk through the inspection of the [X/Fe]-age relations of 24 species from C to Eu. Methods: Using high-resolution and high-signal-to-noise UVES spectra of nine solar twins, we obtained precise estimates of stellar ages and chemical abundances. These determinations have been integrated with additional accurate age and abundance determinations from recent spectroscopic studies of solar twins existing in the literature, comprising superb abundances with 0.01~dex precision. Based on this data set, we outlined the [X/Fe]-age relations over a time interval of 10~Gyr. Results: We present the [X/Fe] - age relations for 24 elements (C, O, Na, Mg, Al, Si, S, K, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, Cu, Zn, Y, Ba, La, Ce, Nd, and Eu). Each different class of elements showed distinct evolution with time that relies on the different characteristics, rates and timescales of the nucleosynthesis' sites from which they are produced. The $α$-elements are characterised by a [X/Fe] decrement as time goes on. Strikingly, an opposite behaviour is observed for Ca. The iron-peak elements show an early [X/Fe] increase followed by a decrease towards the youngest stars. The [X/Fe] for the n-capture elements decrease with age. We also found that both [Mg/Y] and [Al/Y] are precise stellar clocks, with [Al/Y] showing the steepest dependence with age. Conslusions: Knowledge of the [X/Fe]-age relations is a gold mine from which we can achieve a great understanding about the processes that governed the formation and evolution of the Milky Way. Through the reverse engineering of these relations we will be able to put strong constraints on the nature of the stellar formation history, the SNe rates, the stellar yields, and the variety of the SNe progenitors.
Infall and Disk Processes - the Message from Meteorites
California Institute of Technology（加州理工学院）；Max Planck Institute for Solar System Research（马克斯·普朗克太阳系统研究所）；American Museum of Natural History（美国自然历史博物馆）；Center for Computational Astrophysics, Flatiron Institute（平顿研究所计算天体物理学中心）；University of Connecticut（康涅狄格大学）；University of Göttingen（哥廷根大学）；University of Copenhagen（哥本哈根大学）
Color-Magnitude Diagram Constraints on the Metallicities, Ages, and Star Formation History of the Stellar Populations in the Carina Dwarf Spheroidal Galaxy
Stellar Population Astrophysics (SPA) with the TNG 23 IR elemental abundances of 114 giant stars in 41 Open Clusters
Malmö University（马尔默大学）；Nordic Optical Telescope（北欧光学望远镜）；University of Rome Tor Vergata（罗马托尔维加塔大学）；INAF-Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚天体物理与空间科学观测站）；Stockholm University（斯德哥尔摩大学）；INAF - Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；Fundacíon Galileo Galilei - INAF（伽利略基金会-意大利国家天体物理研究所）
