Hydrodynamical simulations of galaxy formation: effects of supernova feedback
Hydrodynamical simulations of galaxy formation: effects of supernova feedback
复制标题
星系形成的流体动力学模拟：超新星反馈的影响
DOI：
10.1093/mnras/284.1.235
复制
发表时间：
1996
影响因子：
4.8
通讯作者：
A. Klypin
中科院分区：
文献类型：
--
作者：
G. Yepes;R. Kates;A. Khokhlov;A. Klypin
我们数值模拟了星系形成中一些最关键的物理过程：超新星反馈，结合气体动力学和重力，在确定星系如何在大尺度结构模型的背景下出现方面起着至关重要的作用。我们的治疗结合了星际介质的多相模型，包括冷却，加热和金属富集超新星的影响，和冷云的蒸发。星星的形成发生在冷气体云的内部，这些气体云是通过热不稳定性产生的。我们在标准偏置CDM模型中模拟了星系的形成过程，在不同的参数和不同的分辨率下（2- 20 $h ^{-1}$kpc）。在我们的图片中，超新星反馈调节气体成分的演化和星星的形成。超新星云蒸发的效率强烈影响星星的形成速率。这种反馈导致大星系（质量大于2 - 3 × 10 ^{11}\Msun$）中星星的形成速率稳定在（1-10）\Msun\yr$的水平，z为-15 $。在大星系和小星系的情况下，发光物质（恒星）的分布相对于暗物质有很大的偏差。我们找到了一个近似的偏置测度，当z=0且密度超过1000时，其形式为$\rho_{lum}=（\rho_{dm}/133）^{1.7}$。偏离这种关系（系数2-3）取决于环境。对于质量超过2 × 10 ^{10}\Msun$的晕，绝对星等与总质量的关系可以近似为M_V=-18.5-4\log（M_{tot}/10^{11}\Msun）$，离散度小于0.5等。
We numerically simulate some of the most critical physical processes in galaxy formation: The supernova feedback, in conjunction with gasdynamics and gravity, plays a crucial role in determining how galaxies arise within the context of a model for large-scale structure. Our treatment incorporates a multi-phase model of the interstellar medium and includes the effects of cooling, heating and metal enrichment by supernovae, and evaporation of cold clouds. The star formation happens inside the clouds of cold gas, which are produced via thermal instability. We simulate the galaxy formation in standard biased CDM model for a variety of parameters and for several resolutions in the range 2--20$h^{-1}$kpc. In our picture, supernova feedback regulates the evolution of the gas components and star formation. The efficiency of cloud evaporation by supernova strongly influences star formation rates. This feedback results in a steady rate of star formation in large galaxies (mass larger than $2-3x10^{11}\Msun$) at a level of $(1-10)\Msun\yr$ for $z -15$. In the case of both large and small galaxies, the distribution of luminous matter (stars) is strongly BIASED with respect to the dark matter. We find an approximate biasing measure of the form $\rho_{lum}= (\rho_{dm}/133)^{1.7}$ for z=0 and overdensities exceeding 1000. Deviations from this relation (a factor 2-3) depend on the environment. For halo masses exceeding $2x10^{10}\Msun$, the dependence of the absolute magnitude on the total mass can be approximated as $M_V=-18.5-4\log(M_{tot}/10^{11}\Msun)$, with a scatter of less than 0.5mag.