Large-eddy simulations of isolated disc galaxies with thermal and turbulent feedback

被引：15
作者：
Braun, H. [1 ]
Schmidt, W. [1 ]
Niemeyer, J. C. [1 ]
Almgren, A. S. [2 ]
机构：
[1] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany
[2] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Ctr Computat Sci & Engn, Berkeley, CA 94720 USA
来源：
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2014年 / 442卷 / 04期
关键词：
turbulence; methods: numerical; stars: formation; galaxies: ISM; STAR-FORMATION RATE; ACCRETION-DRIVEN TURBULENCE; GIANT MOLECULAR CLOUDS; GAS DEPLETION TIME; INTERSTELLAR-MEDIUM; FORMATION LAW; GRAVITATIONAL-INSTABILITY; NUMERICAL-SIMULATION; FORMATION EFFICIENCY; GALACTIC TURBULENCE;
D O I：
10.1093/mnras/stu1119
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We present a subgrid-scale model for the Multi-phase Interstellar medium, Star formation, and Turbulence (MIST) and explore its behaviour in high-resolution large-eddy simulations of isolated disc galaxies. MIST follows the evolution of a clumpy cold and a diffuse warm component of the gas within a volume element which exchange mass and energy via various cooling, heating and mixing processes. The star formation rate is dynamically computed from the state of the gas in the cold phase. An important feature of MIST is the treatment of unresolved turbulence in the two phases and its interaction with star formation and feedback by supernovae. This makes MIST a particularly suitable model for the interstellar medium in galaxy simulations. We carried out a suite of simulations varying fundamental parameters of our feedback implementation. Several observational properties of galactic star formation are reproduced in our simulations, such as an average star formation efficiency similar to 1 per cent, a typical velocity dispersion around similar to 10 km s(-1) in star-forming regions, and an almost linear relationship between the column densities of star formation and dense molecular gas.
引用
收藏
页码：3407 / 3426
页数：20
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