星系演化模拟中分子氢依赖的恒星形成模型
A model for molecular hydrogen-dependent star formation in simulations of galaxy evolution
AI总结：
本研究提出一种适用于流体动力学模拟的新型恒星形成模型，通过描述从原子物质形成分子氢的过程并考虑化学丰度依赖，比较了基于原子和/或分子气相的SFR预测与观测结果。
摘要：
恒星形成及其相关的化学和能量反馈是星系演化中最重要的过程之一。星系中的恒星形成活动决定并影响其许多基本性质，如恒星质量、形态和化学富集水平。宇宙学流体动力学模拟中的简单恒星形成模型已被证明在重现不同类型星系的恒星形成率（SFR）水平和形状方面是成功的。然而，随着高分辨率模拟和更详细观测的出现，需要更复杂的恒星形成模型；特别是为了更好地理解恒星形成与原子和分子相气体量之间的关系。在这项工作中，我们将最近开发的、适用于流体动力学模拟背景的新型恒星形成模型应用于银河系质量星系SFR的研究。该新实现描述了从原子物质形成分子氢的过程，同时考虑了与气体化学丰度的可能依赖关系。这使得能够实现各种恒星形成模型，其中气体云的SFR由原子和/或分子气相决定，并将其预测与最近的观测结果进行比较。
英文摘要：
Star formation, together with the associated chemical and energy feedback, is one of the most important processes in galaxy evolution. The star formation activity in galaxies defines and affects many of their fundamental properties, such as stellar mass, morphology and chemical enrichment levels. Simple models for star formation in cosmological hydrodynamical simulations have shown to be successful in reproducing the star formation rate (SFR) levels and shapes of different types of galaxies. However, with the advent of high-resolution simulations and more detailed observations, more sophisticated star formation models are needed; in particular, to better understand the relation between star formation and the amount of gas in the atomic and molecular phases. In this work, we apply a novel star formation model, recently developed to work in the context of hydrodynamical simulations, to the study of the SFR in Milky Way-mass galaxies. The new implementation describes the formation of molecular hydrogen from atomic material, considering also possible dependencies with the chemical abundance of the gas. This allows to implement various star formation models, where the SFR of a gas cloud is determined by the atomic and/or molecular gas phases, and to compare their predictions to recent observational results.
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