论文标题
Lyra I：模拟具有各个星星的矮星系的多相ISM
LYRA I: Simulating the multi-phase ISM of a dwarf galaxy with variable energy supernovae from individual stars
论文作者
论文摘要
我们介绍了Lyra Project，这是一种建立在宇宙学水力学移动网格代码框架内的新的高分辨率星系组模型。该模型将多相星际培养基解析至10K。它形成了从初始质量函数（IMF）采样的单个星星，并单独跟踪其寿命和死亡途径。在流体动力计算中遵循具有可变能量的单个超新星（SN）爆炸波，以与周围的星际介质（ISM）相互作用。在本文中，我们介绍了方法，并将模型应用于$ 10^{10} m _ {\ odot} $隔离晕。我们证明，大多数超新星在我们的基准气体质量分辨率为$ 4 m _ {\ odot} $上是通过SEDOV解决的。我们表明，我们的SN反馈处方自一致地在ISM中产生一个热相，驱动大量流出，降低气体密度并抑制恒星形成。聚集的SN在增强反馈的有效性方面起着重要作用，因为大多数爆炸发生在低密度材料中。核算可变的SN能量可以使反馈直接响应恒星演化。我们表明ISM对空间分布的能量沉积敏感。它强烈影响流出行为，将质量负荷减少2-3，从而使银河系保留了较高的质量和金属。 Lyra可以直接在识别和较高的质量星系的宇宙学（变焦）模拟中使用综合的多物理ISM模型。
We introduce the LYRA project, a new high resolution galaxy formation model built within the framework of the cosmological hydro-dynamical moving mesh code AREPO. The model resolves the multi-phase interstellar medium down to 10 K. It forms individual stars sampled from the initial mass function (IMF), and tracks their lifetimes and death pathways individually. Single supernova (SN) blast waves with variable energy are followed within the hydrodynamic calculation to interact with the surrounding interstellar medium (ISM). In this paper, we present the methods and apply the model to a $10^{10} M_{\odot}$ isolated halo. We demonstrate that the majority of supernovae are Sedov-resolved at our fiducial gas mass resolution of $4 M_{\odot}$. We show that our SN feedback prescription self-consistently produces a hot phase within the ISM that drives significant outflows, reduces the gas density and suppresses star formation. Clustered SN play a major role in enhancing the effectiveness of feedback, because the majority of explosions occur in low density material. Accounting for variable SN energy allows the feedback to respond directly to stellar evolution. We show that the ISM is sensitive to the spatially distributed energy deposition. It strongly affects the outflow behaviour, reducing the mass loading by a factor of 2-3, thus allowing the galaxy to retain a higher fraction of mass and metals. LYRA makes it possible to use a comprehensive multi-physics ISM model directly in cosmological (zoom) simulations of dwarf and higher mass galaxies.
