The Galactic Bulge can uniquely be studied from large samples of individual stars, and is therefore of prime importance for understanding the stellar population structure of bulges in general. Here the observational evidence on the kinematics, chemical composition, and ages of Bulge stellar populations based on photometric and spectroscopic data is reviewed. The bulk of Bulge stars are old and span a metallicity range -1.5<~[Fe/H]<~+0.5. Stellar populations and chemical properties suggest a star formation timescale below ~2 Gyr. The overall Bulge is barred and follows cylindrical rotation, and the more metal-rich stars trace a Box/Peanut (B/P) structure. Dynamical models demonstrate the different spatial and orbital distributions of metal-rich and metal-poor stars. We discuss current Bulge formation scenarios based on dynamical, chemical, chemodynamical and cosmological models. Despite impressive progress we do not yet have a successful fully self-consistent chemodynamical Bulge model in the cosmological framework, and we will also need more extensive chrono-chemical-kinematic 3D map of stars to better constrain such models.

中文翻译：

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银河系隆起的化学动力学史

银河凸起可以从单个恒星的大量样本中进行独特的研究，因此对于了解一般凸起的恒星群结构至关重要。这里回顾了基于光度和光谱数据的关于膨胀星族的运动学、化学成分和年龄的观测证据。大部分的凸出星都很古老，金属丰度范围为 -1.5<~[Fe​​/H]<~+0.5。恒星数量和化学性质表明恒星形成的时间尺度低于~2 Gyr。整体的凸起被禁止并遵循圆柱形旋转，而富含金属的恒星则呈现出盒/花生 (B/P) 结构。动力学模型展示了富金属和贫金属恒星的不同空间和轨道分布。我们讨论了基于动力学、化学、化学动力学和宇宙学模型。尽管取得了令人瞩目的进展，但在宇宙学框架中，我们还没有一个成功的完全自洽的化学动力学凸起模型，我们还需要更广泛的恒星时间-化学-运动学 3D 图来更好地约束这些模型。