论文标题
一个随机模型，用于在流体动力学模拟中重现单个星系的恒星形成史
A stochastic model to reproduce the star-formation history of individual galaxies in hydrodynamic simulations
论文作者
论文摘要
星系的恒星形成历史（SFH）对于理解星系进化至关重要。流体动力学模拟使我们能够精确地重建星系的SFH，并建立与潜在物理过程的链接。在这项工作中，我们提出了一个模型，以描述三个模拟的单个星系的SFH：Thethreehuntive，Illustris-1和TNG100-1。该模型将银河系SFH分为两个不同的组成部分：“主序列”和“变化”。 “主序列”部分是通过追踪跨时间的$ sfr-m _*$主序列的历史而生成的。 “变异”部分由主序列周围的散射组成，该序列由分数布朗动作重现。我们发现：1）主序列的演变在模拟之间有所不同； 2）分数布朗动作可以再现SFH的许多特征，但是，仍然存在差异。 3）变化和质量损失率对于重建模拟的SFH至关重要。该模型在模拟中提供了对SFHS的公平描述。另一方面，通过将分数布朗运动模型与模拟数据相关联，我们提供了一个“标准”，以比较模拟。
The star formation history (SFH) of galaxies is critical for understanding galaxy evolution. Hydrodynamical simulations enable us to precisely reconstruct the SFH of galaxies and establish a link to the underlying physical processes. In this work, we present a model to describe individual galaxies' SFHs from three simulations: TheThreeHundred, Illustris-1 and TNG100-1. This model divides the galaxy SFH into two distinct components: the "main sequence" and the "variation". The "main sequence" part is generated by tracing the history of the $SFR-M_*$ main sequence of galaxies across time. The "variation" part consists of the scatter around the main sequence, which is reproduced by fractional Brownian motions. We find that: 1) The evolution of the main sequence varies between simulations; 2) fractional Brownian motions can reproduce many features of SFHs, however, discrepancies still exist; 3) The variations and mass-loss rate are crucial for reconstructing the SFHs of the simulations. This model provides a fair description of the SFHs in simulations. On the other hand, by correlating the fractional Brownian motion model to simulation data, we provide a 'standard' against which to compare simulations.
