Star formation is a multi-scale, multi-physics problem ranging from the size scale of molecular clouds ( ∼ 10 ${\sim} 10$ s pc) down to the size scales of dense prestellar cores ( ∼ 0.1 ${\sim} 0.1$ pc) that are the birth sites of stars. Several physical processes like turbulence, magnetic fields and stellar feedback, such as radiation pressure and outflows, are more or less important for different stellar masses and size scales. During the last decade a variety of technological and computing advances have transformed our understanding of star formation through the use of multi-wavelength observations, large scale observational surveys, and multi-physics multi-dimensional numerical simulations. Additionally, the use of synthetic observations of simulations have provided a useful tool to interpret observational data and evaluate the importance of various physical processes on different scales in star formation. Here, we review these recent advancements in both high- ( M ≳ 8 M ⊙ $M \gtrsim 8~M_{\odot }$ ) and low-mass star formation.

中文翻译：

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放大单个恒星的形成：低质量和高质量的恒星

恒星形成是一个多尺度、多物理的问题，从分子云的大小尺度（~ 10 ${\sim} 10$ s pc）到致密的前星核的大小尺度（~ 0.1 ${\sim} 0.1$ pc) 是恒星的诞生地。一些物理过程，如湍流、磁场和恒星反馈，如辐射压力和外流，对不同的恒星质量和大小尺度或多或少都很重要。在过去十年中，通过使用多波长观测、大规模观测调查和多物理多维数值模拟，各种技术和计算的进步改变了我们对恒星形成的理解。此外，模拟合成观测的使用为解释观测数据和评估恒星形成过程中不同尺度的各种物理过程的重要性提供了有用的工具。在这里，我们回顾了这些在高质量（M ≳ 8 M ⊙ $M \gtrsim 8~M_{\odot }$ ）和低质量恒星形成方面的最新进展。