Integrated Models of Magnetic Fields and Gas Kinematics in Molecular Clouds

分子云中磁场和气体运动学的集成模型

• 批准号: RGPIN-2017-05930
• 负责人: Fiege, Jason
• 金额: $ 1.53万
• 依托单位: University of Manitoba
• 依托单位国家: 加拿大
• 项目类别: Discovery Grants Program - Individual
• 财政年份: 2017
• 资助国家: 加拿大
• 起止时间: 2017-01-01 至 2018-12-31
• 项目状态: 已结题
• 来源: https://www.nserc-crsng.gc.ca/ase-oro/Details-Detailles_eng.asp?id=633422
• 关键词: Integrated; Models; Magnetic; Fields; Gas

Molecular clouds are magnetized, turbulent, self-gravitating structures, and the seat of star formation in our Galaxy. Star formation occurs on small scales (~0.1 pc), in dense cores, where gravity overcomes turbulence and outward magnetic forces. Magneto-centrifugal forces drive a pair of jets, which sweep up surrounding gas into a pair of bipolar molecular outflows. Self-gravity, outflows, and magnetic fields are strongly coupled in star formation.

分子云是磁化的、湍流的、自引力的结构，是我们银河系中星星形成的所在地。 星星的形成发生在小尺度（~0.1秒差距）的致密核心中，那里的重力克服了湍流和向外的磁力。 磁离心力驱动一对射流，将周围的气体扫入一对双极分子外流。 在星星的形成过程中，自引力、外流和磁场是强耦合的。