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arXiv 1902.05744astro-ph.GAastro-ph.SR
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大质量坍缩暗条中的核心和恒星质量函数

The core and stellar mass functions in massive collapsing filaments

Evangelia Ntormousi, Patrick Hennebelle

备注：
Accepted for publication by A&A
发表信息：
A&A 625, A82 (2019)
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摘要：

星前核心质量函数（CMF）和恒星初始质量函数（IMF）之间的联系是所有恒星形成理论的核心。在本文中，我们研究了恒星形成的最早阶段与一系列高分辨率的数值模拟，包括形成的汇。特别是，我们专注于从核心的过渡到一个巨大的分子丝内的水槽。我们比较CMF和IMF磁化和未磁化的模拟，以及不同的分辨率之间。我们发现，选择核心的基础上，他们的运动维里参数排除崩溃的对象，因为他们主机大的速度分散。只选择热不稳定的磁化核心，我们观察到，他们的质量-通量比跨越几乎两个数量级的给定质量。我们还看到，当包括磁场，CMF峰值在较高的核心质量值相对于纯流体动力学模拟。尽管如此，所有的模型都产生了与萨尔彼得一致的高质量斜率的下沉质量函数。最后，我们检查了分辨率的影响，并发现在等温模拟中，即使是动态范围非常高的模型也无法在质量函数中收敛。我们的主要结论是，虽然所得到的CMFs和IMF在所有模拟中具有相似的斜率，但当包括磁场时，芯的尺寸和运动学性质略有不同。然而，如果我们不考虑热稳定性，仅仅基于质量通量比的核心选择不足以改变CMF的形状。最后，我们得出结论，极端小心应给予解决问题时，研究汇的形成与等温状态方程。

英文摘要：

The connection between the pre-stellar core mass function (CMF) and the stellar initial mass function (IMF) lies at the heart of all star formation theories. In this paper, we study the earliest phases of star formation with a series of high-resolution numerical simulations that include the formation of sinks. In particular, we focus on the transition from cores to sinks within a massive molecular filament. We compare the CMF and IMF between magnetized and unmagnetized simulations, and between different resolutions. We find that selecting cores based on their kinematic virial parameter excludes collapsing objects because they host large velocity dispersions. Selecting only the thermally unstable magnetized cores, we observe that their mass-to-flux ratio spans almost two orders of magnitude for a given mass. We also see that, when magnetic fields are included, the CMF peaks at higher core mass values with respect to pure hydrodynamical simulations. Nonetheless, all models produce sink mass functions with a high-mass slope consistent with Salpeter. Finally, we examine the effects of resolution and find that, in isothermal simulations, even models with very high dynamical range fail to converge in the mass function. Our main conclusion is that, although the resulting CMFs and IMFs have similar slopes in all simulations, the cores have slightly different sizes and kinematical properties when a magnetic field is included. However, a core selection based on the mass-to-flux ratio alone is not enough to alter the shape of the CMF, if we do not take thermal stability into account. Finally, we conclude that extreme care should be given to resolution issues when studying sink formation with an isothermal equation of state.

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