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arXiv 2604.11642astro-ph.EPastro-ph.SR
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基于其质量统计分析的原行星盘引力稳定性的研究

Investigation of gravitational stability of protoplanetary disks based on statistical analysis of their masses

Saint Petersburg State University（圣彼得堡国立大学）

Sophia A. Drobchik, Sergey A. Khaibrakhmanov

备注：
Accepted to Astronomy Reports, 10 pages, 3 figures, 2 tables, 1 Appendix
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AI总结：

通过统计分析原行星盘质量分布，发现仅1.2%的盘处于不稳定状态，可能由于观测方法的系统性低估导致理论预期不符。

摘要：

我们收集了1155个原行星盘的数据，结合十项恒星形成区域的调查数据。基于该样本，我们构建了盘质量分布的幂律近似：dN/dM ∝ M^{-β}，β=1.36±0.14。我们利用该样本对原行星盘的引力稳定性进行了统计分析。为了分析盘的稳定性，我们计算了每个盘的Toomre参数（Q）。在计算中假设盘的径向密度分布由幂律分布描述。Toomre参数的计算显示，样本中仅1.2%的盘正式不稳定（Q < 1），而1.7%的盘处于边缘稳定性状态（1 ≤ Q ≤ 2）。观测到的不稳定盘数量较少与理论预期相矛盾，可能由于观测方法的局限性导致盘质量的系统性低估。考虑到光学深度、CO耗尽以及气体-尘埃比的不确定性，我们得出结论，实际处于引力不稳定状态的系统比例可能显著更高。

英文摘要：

We compiled a sample of $1155$ protoplanetary disks, combining data from ten surveys of star-forming regions. Based on the sample, we constructed a power-law approximation of the disk mass distribution: $dN/dM \propto M^{-β}$, $β= 1.36 \pm 0.14$. We used the sample for a statistical analysis of the gravitational stability of protoplanetary disks. To analyze the stability of the disks, we calculated the Toomre parameter ($Q$) for each of them. In the calculations, it was assumed that the radial density distribution in the disks is described by a power-law profile. The calculations of the Toomre parameter show that only $1.2$ % of the disks in the sample are formally unstable ($Q < 1$), while $1.7$ % are in a state of marginal stability ($1 \leq Q \leq 2$). The low observed abundance of unstable disks contradicts theoretical expectations and may be explained by a systematic underestimation of disk masses due to limitations of observational methods. Considering the effects of optical depth, CO depletion, as well as uncertainty in the gas-to-dust ratio, we conclude that the actual fraction of the gravitationally unstable systems may be significantly higher.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

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