论文标题
云芯中的恒星形成 - 密集分子核的模拟和观察以及太阳质量恒星的形成
Star formation in cloud cores -- simulations and observations of dense molecular cores and the formation of solar mass stars
论文作者
论文摘要
恒星形成效率低下。分子云的数值模拟和理论模型的最新进展表明，星际湍流，磁场和恒星反馈的综合作用可以解释恒星形成的低效率。恒星形成速率对湍流的驱动方式高度敏感。与螺旋 - AM云中更紧密的驱动剂相比，在中央分子区域中，螺线管驱动可能更重要。理论和观察性努力都在进行，以确定不同银河环境中湍流的主要驱动方式。 ALMA的新观察结果与Carma，JCMT和SMA等其他仪器结合起来，开始揭示密集核心和原始磁盘的磁场结构，显示出具有有序和湍流场成分的高度复杂的场几何形状。这种复杂的磁场可以产生一系列恒星质量和密集核心和原恒星增生磁盘的射流/流出效率。
Star formation is inefficient. Recent advances in numerical simulations and theoretical models of molecular clouds show that the combined effects of interstellar turbulence, magnetic fields and stellar feedback can explain the low efficiency of star formation. The star formation rate is highly sensitive to the driving mode of the turbulence. Solenoidal driving may be more important in the Central Molecular Zone, compared to more compressive driving agents in spiral-am clouds. Both theoretical and observational efforts are underway to determine the dominant driving mode of turbulence in different Galactic environments. New observations with ALMA, combined with other instruments such as CARMA, JCMT and the SMA begin to reveal the magnetic field structure of dense cores and protostellar disks, showing highly complex field geometries with ordered and turbulent field components. Such complex magnetic fields can give rise to a range of stellar masses and jet/outflow efficiencies in dense cores and protostellar accretion disks.
