报告人简介：吕行，现为上海天文台副研究员，研究方向为利用ALMA、SMA、JVLA等射电和亚毫米波干涉仪观测银河系内分子云中的恒星形成活动。2016年获得南京大学天体物理学博士学位并获得江苏省优秀博士论文，期间于2012年3月至2015年8月在美国哈佛-史密森天体物理中心以SMA博士前学者身份从事研究。2016年至2021年在日本国立天文台ALMA项目组担任博士后特任研究员，参与了ALMA实地观测、科学目标规划、观测申请评审等任务。在ApJ，ApJL，ApJS等杂志发表第一作者论文9篇，先后4次获得ALMA最高优先级（A级，占所有项目前5%）的PI观测时间，包括最长基线（16千米）、高频（~460 GHz）、偏振观测等高风险、高回报的挑战性项目，相关成果多次获得ALMA天文台、日本国立天文台、Nature网站、NSF网站等媒体报道。

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Abstract: Star formation is fundamental to all fields of astrophysics; however, there are still many unsettled questions even for star formation in our own Galaxy. I will introduce our recent results about star formation in two different environments in the Galaxy, including filamentary clouds in the Galactic disk and massive molecular clouds in the Central Molecular Zone around the Galactic Center, by using data from my PI ALMA projects. In the filamentary clouds, we focus on gas fragmentation and accretion. We have resolved the clouds into hundreds of 0.01-pc scale 'condensations' and detected signatures of star formation including outflows, hot molecular cores, HII regions, and masers. In the Central Molecular Zone clouds, we set out to explain their low star formation efficiency and find that the root must be related to microscopic physical conditions in pc-scale clouds, while star formation within 0.1-pc scale dense cores proceeds as normal. Finally, I attempt to compare star formation properties in these two environments, including the core mass function, protostellar disk properties, and shock chemistry, and suggest that we can use the results to explain similar variations of star formation efficiencies in external galaxies.

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