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arXiv 1806.01033astro-ph.SRastro-ph.GA
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恒星性质对初始云密度的依赖性

The dependence of stellar properties on initial cloud density

Michael O. Jones, Matthew. R. Bate

备注：
Accepted for publication in MNRAS, 14 pages, 8 figures
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摘要：

我们调查的依赖性的恒星性质的初始平均密度的分子云，其中星团形式使用辐射流体动力学模拟，解决不透明度限制的碎片。我们已经模拟了三个星团的形成，这些星团是由分子云的引力坍缩形成的，这些分子云的密度相差一百倍。与以前的计算，包括辐射反馈，我们发现，依赖的特征恒星质量，$M_{\rm c}$，对云的初始平均密度，$ρ$，是弱于热金斯质量的依赖。然而，与以前的计算，发现没有统计上显着的变化，在密度的中位数质量，我们发现一个弱的依赖性近似的形式$M_{\rm c} \propto ρ^{-1/5}$。多个系统的属性分布在计算之间没有显著变化。我们将我们的结果与恒星形成区域的观测调查结果进行比较，并建议我们的最低密度计算和附近的金牛座-御夫座区域的性质之间的相似性表明，观测到的太阳型恒星明显过剩可能是由于该区域的低密度。

英文摘要：

We investigate the dependence of stellar properties on the initial mean density of the molecular cloud in which stellar clusters form using radiation hydrodynamical simulations that resolve the opacity limit for fragmentation. We have simulated the formation of three star clusters from the gravitational collapse of molecular clouds whose densities vary by a factor of a hundred. As with previous calculations including radiative feedback, we find that the dependence of the characteristic stellar mass, $M_{\rm c}$, on the initial mean density of the cloud, $ρ$, is weaker than the dependence of the thermal Jeans mass. However, unlike previous calculations, which found no statistically significant variation in the median mass with density, we find a weak dependence approximately of the form $M_{\rm c} \propto ρ^{-1/5}$. The distributions of properties of multiple systems do not vary significantly between the calculations. We compare our results to the result of observational surveys of star-forming regions, and suggest that the similarities between the properties of our lowest density calculation and the nearby Taurus-Auriga region indicate that the apparent excess of solar-type stars observed may be due to the region's low density.

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