论文标题
大型麦哲伦云质量模拟星系中多相银河风的结构和组成
The structure and composition of multiphase galactic winds in a Large Magellanic Cloud mass simulated galaxy
论文作者
论文摘要
我们提出了高分辨率模拟的第一个结果，重点是银河系驱动银河系，其光环质量为$ \ sim 10^{11} $ m $ _ {\ odot} $（类似于大麦芽岩云），总气体质量为$ \ sim 6 \ sim 6 \ sim times 10^{8} $ m $ m $ _ $ _} $ _} $ \ sim 4 $ m $ _ {\ odot} $质量分辨率的10^{8} $气体单元。我们采用了一种已解决的恒星反馈模型，具有非平衡冷却和加热，包括光电加热和光电子辐射，以及超新星（SNE），与二阶网格无线有限质量（MFM）方法耦合。这些功能使其成为迄今为止运行的最大的解析 - 星系模型。 We find mean star formation rates around $0.05$ M$_{\odot}$ yr$^{-1}$ and evaluate typical time averaged loading factors for mass ($η_\mathrm{M}$ $\sim$ 1.0, in good agreement with recent observations) and energy ($η_\mathrm{E}$ $\sim$ 0.01).风的大部分质量是由温暖（$ t <5 \ times 10^5 $ k）阶段传输的，而温暖和热阶段（$ t> 5 \ times 10^5 $ k）在温暖和热阶段中运输了相似的能量。我们发现风的平均开口角为30度，降低，高度高于中平面。对于温暖（热）阶段的风量载荷是恒星形成率密度$σ_ {\ rm sfr} $的函数的函数，而能量负载则显示出$σ_{\ rm sfr} $的倒置趋势，降低了热风，降低了热风，尽管非常有光泽，但它的趋势是非常有益的。这些量表与以前对多相ISM中解决的风能驱动的模拟非常吻合。
We present the first results from a high resolution simulation with a focus on galactic wind driving for an isolated galaxy with a halo mass of $\sim 10^{11}$ M$_{\odot}$ (similar to the Large Magellanic Cloud) and a total gas mass of $\sim 6 \times 10^{8}$ M$_{\odot}$, resulting in $\sim 10^{8}$ gas cells at $\sim 4$ M$_{\odot}$ mass resolution. We adopt a resolved stellar feedback model with non-equilibrium cooling and heating, including photoelectric heating and photo-ionizing radiation, as well as supernovae (SNe), coupled to the second order meshless finite mass (MFM) method for hydrodynamics. These features make this the largest resolved-ISM galaxy model run to date. We find mean star formation rates around $0.05$ M$_{\odot}$ yr$^{-1}$ and evaluate typical time averaged loading factors for mass ($η_\mathrm{M}$ $\sim$ 1.0, in good agreement with recent observations) and energy ($η_\mathrm{E}$ $\sim$ 0.01). The bulk of the mass of the wind is transported by the warm ($T < 5 \times 10^5$K) phase, while there is a similar amount of energy transported in the warm and the hot phases ($T > 5 \times 10^5$K). We find an average opening angle of 30 degrees for the wind, decreasing with higher altitude above the midplane. The wind mass loading is decreasing (flat) for the warm (hot) phase as a function of the star formation surface rate density $Σ_{\rm SFR}$, while the energy loading shows inverted trends with $Σ_{\rm SFR}$, decreasing for the warm wind and increasing for the hot wind, although with very shallow slopes. These scalings are in good agreement with previous simulations of resolved wind driving in the multi-phase ISM.
