报告人：马祥程  （加州理工大学）

时间：2015年9月17日下午4：00

地点：东区理化大楼18层天文台报告厅

报告摘要：I will briefly introduce the FIRE project, which is a suite of cosmological zoom-in simulations using a full set of explicit multi-phase ISM, star formation, and stellar feedback models. These simulations require no need to tune free parameters, but can successfully reproduce a number of observed galaxy properties: the stellar mass-halo mass relation, the Kennicutt-Schmidt law, the star-forming main sequence, star formation histories, etc. (Hopkins et al., 2014, MNRAS, 445, 581). We use these simulations to predict the shape and evolution of the galaxy mass-metallicity relation. I will compare our results with observations and other theoretical models and discuss the key factors that affect galactic chemical evolution but have not been well appreciated by the community (Ma et al., 2015, MNRAS, in press, arxiv:1504.02097). I will also talk about a result I have published on the escape fraction of hydrogen ionizing photons from high-redshift galaxies in the FIRE simulations and discuss its implication on reionization (Ma et al., 2015, MNRAS, 453, 960).