论文标题
部分可观测时空混沌系统的无模型预测
The Effect of Shock Wave Duration on Star Formation and the Initial Condition of Massive Cluster Formation
论文作者
论文摘要
恒星以致密的分子丝出生，无论其质量如何。冲击对ISM的压缩会导致分子云中的细丝形成。观察结果表明，在云中气柱密度的峰值超过10^23 cm^-2时，发生了巨大的恒星簇形成。在这项研究中，我们研究了冲击压缩层持续时间对细丝/恒星形成的影响，以及如何通过执行三维（3D）等温磁性水力动力学（MHD）模拟来实现大规模恒星形成的初始条件，并使用{{over the bass a the Borgaries from {over the Borgaries from {over the Borgations}（即冲击波浪持续时间）作为控制参数。短持续时间在短时间冲击持续时间模型后持续时间膨胀后，形成的细丝会扩展，而长持续时间模型通过形成大量的超临界细丝而导致恒星形成。此外，当电击持续时间长于两个自由下落的时间时，压缩层的峰柱密度超过10^23 cm^-2，并且{{层的重力塌陷}}}}的重力塌陷}预计在冲击压缩层中形成的OB恒星数量达到十个阶数（即，质量群集组成）。
Stars are born in dense molecular filaments irrespective of their mass. Compression of the ISM by shocks cause filament formation in molecular clouds. Observations show that a massive star cluster formation occurs where the peak of gas column density in a cloud exceeds 10^23 cm^-2. In this study, we investigate the effect of the shock-compressed layer duration on filament/star formation and how the initial conditions of massive star formation are realized by performing three-dimensional (3D) isothermal magnetohydrodynamics (MHD) simulations with {gas inflow duration from the boundaries (i.e., shock wave duration)} as a controlling parameter. Filaments formed behind the shock expand after the duration time for short shock duration models, whereas long duration models lead to star formation by forming massive supercritical filaments. Moreover, when the shock duration is longer than two postshock free-fall times, the peak column density of the compressed layer exceeds 10^23 cm^-2, and {the gravitational collapse of the layer causes that} the number of OB stars expected to be formed in the shock-compressed layer reaches the order of ten (i.e., massive cluster formation).
