论文标题
大量原始g31.41+0.31中的尖锐的阿尔玛（Alma）视图
The sharp ALMA view of infall and outflow in the massive protocluster G31.41+0.31
论文作者
论文摘要
语境。为了更好地理解高质量恒星的形成，研究物质如何积聚到年轻的大型恒星，弹出方式以及所有这些与低质量案例有何不同是至关重要的。 The massive protocluster G31.41+0.31 is the ideal target to study all these processes because observations at millimeter and centimeter wavelengths have resolved the emission of the Main core into at least four massive dust continuum sources, named A, B, C, and D, within 1" or 0.018 pc, and have identified signatures of infall and several outflows associated with the core. Aims. We study the interplay between通过在数量100 au的空间分辨率上研究其特性及其对核心方法的影响，我们进行了典型的高密度示踪剂（例如CH3CN或H2CO），以及诸如An0 An n0 and s s s s s s s s s s s s s s s s， au）。结果。这些观察结果表明，CH3CN和H2CO中的P-CygNI谱图朝向主要核心中的四个来源，这表明所有这些来源都在崩溃。从红移的吸收中估计的插入率在1E-2 MSUN/年的阶。单个内部速率表明，主要核心的积聚时间尺度比其旋转时间尺度小的数量级。这证实了旋转的环形旋转的旋转环芯是非平衡的瞬态崩溃结构，需要不断地用大规模储层的新鲜材料补充。对于来源B，C和D，该中心可能会在源内加速，而对于来源A，第二发射成分的存在使解释变得复杂。 SIO观察结果表明，G31.41+0.31星形成区域中至少存在六个流出。
Context. To better understand the formation of high-mass stars, it is fundamental to investigate how matter accretes onto young massive stars, how it is ejected, and how all this differs from the low-mass case. The massive protocluster G31.41+0.31 is the ideal target to study all these processes because observations at millimeter and centimeter wavelengths have resolved the emission of the Main core into at least four massive dust continuum sources, named A, B, C, and D, within 1" or 0.018 pc, and have identified signatures of infall and several outflows associated with the core. Aims. We study the interplay between infall and outflow in G31.41+0.31 by investigating at a spatial resolution of a few 100 au their properties and their possible impact on the core. Methods. We carried out molecular line observations of typical high-density tracers, such as CH3CN or H2CO, and shock and outflow tracers, such as SiO, with ALMA at 1.4 mm that achieved an angular resolution of 0.09" (340 au). Results. The observations have revealed inverse P-Cygni profiles in CH3CN and H2CO toward the four sources embedded in the Main core, suggesting that all of them are undergoing collapse. The infall rates, estimated from the red-shifted absorption are on the order of 1E-2 Msun/yr. The individual infall rates imply that the accretion timescale of the Main core is an order of magnitude smaller than its rotation timescale. This confirms that rotating toroids such as the G31 Main core are non-equilibrium, transient collapsing structures that need to be constantly replenished with fresh material from a large-scale reservoir. For sources B, C, and D, the infall could be accelerating inside the sources, while for source A, the presence of a second emission component complicates the interpretation. The SiO observations have revealed the presence of at least six outflows in the G31.41+0.31 star-forming region, ...
