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arXiv 2407.21101astro-ph.EPastro-ph.SR
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$M_{\mathrm{d}}-M_{\star}$与$\dot M-M_{\star}$相关性的演化追踪原行星盘的消散

The evolution of the $M_{\mathrm{d}}-M_{\star}$ and $\dot M-M_{\star}$ correlations traces protoplanetary disc dispersal

Alice Somigliana, Leonardo Testi, Giovanni Rosotti, Claudia Toci, Giuseppe Lodato, Rossella Anania, Benoît Tabone, Marco Tazzari, Ralf Klessen, Ugo Lebreuilly, … 展开作者

Alice Somigliana, Leonardo Testi, Giovanni Rosotti, Claudia Toci, Giuseppe Lodato, Rossella Anania, Benoît Tabone, Marco Tazzari, Ralf Klessen, Ugo Lebreuilly, Patrick Hennebelle, Sergio Molinari

备注：
14 pages, 5 figures and 3 tables (plus Appendix). Accepted for publication in A&A. Includes Diskpop and popcorn software release
发表信息：
A&A 689, A285 (2024)
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AI总结：

研究通过分析计算与Diskpop模拟探讨风驱动和混合情形下盘性质与恒星质量幂律斜率的演化，发现MHD风改变相关性形状，增加样本量可揭示盘演化驱动机制。

摘要：

（节选）对整个恒星形成区的观测巡天提供了盘性质与恒星质量之间存在幂律相关性的证据，特别是盘质量（${M_d \propto M_*}^{λ_m}$）和吸积率（$\dot M \propto {M_*}^{λ_{acc}}$）。长期盘演化是否影响上述相关性仍存在争议：虽然纯粘性情景已被探讨，但其他机制可能会产生不同的影响。我们研究了风驱动和混合情形下斜率$λ_m$和$λ_{acc}$的演化，并将其与粘性预测进行比较，使用了分析计算和数值模拟（使用1D种群合成代码Diskpop执行，我们也在此发布该代码）相结合的方法。假设$M_d(0) \propto {M_*}^{λ_{m, 0}}$和$\dot M(0) \propto {M_*}^{λ_{acc, 0}}$作为初始条件，我们发现粘性和混合吸积保持了相关性的形状并演化其斜率；另一方面，MHD风改变了相关性的形状，根据吸积时间尺度与恒星质量的标度关系使其弯曲。我们还展示了初始条件中的离散如何掩盖这一行为。随后我们分析了盘消散的影响，发现当前可用的样本量（5 Myr时约30个盘）在斜率演化中引入了随机振荡，这主导了物理特征。增加样本量可以缓解此问题：5 Myr时约140个盘，对应完整的Upper Sco样本，将提供足够小的误差棒，从而将斜率演化用作盘演化驱动机制的代理。最后，我们讨论了斜率变陡的观测主张如何必然导致初始$M_d - M_*$相关性比$\dot M - M_*$更陡峭。

英文摘要：

(Abridged) Observational surveys of entire star-forming regions have provided evidence of power-law correlations between the disc properties and the stellar mass, especially the disc mass (${M_d \propto M_*}^{λ_m}$) and the accretion rate ($\dot M \propto {M_*}^{λ_{acc}}$). Whether the secular disc evolution affects said correlations is still debated: while the purely viscous scenario has been probed, other mechanisms could impact differently. We study the evolution of the slopes $λ_m$ and $λ_{acc}$ in the wind-driven and hybrid case and compare it to the viscous prediction, using a combination of analytical calculations and numerical simulations (performed with the 1D population synthesis code Diskpop, that we also present and release). Assuming $M_d(0) \propto {M_*}^{λ_{m, 0}}$ and $\dot M(0) \propto {M_*}^{λ_{acc, 0}}$ as initial conditions, we find that viscous and hybrid accretion preserve the shape of the correlations and evolve their slope; on the other hand, MHD winds change the shape of the correlations, bending them according to the scaling of the accretion timescale with the stellar mass. We also show how a spread in the initial conditions conceals this behaviour. We then analyse the impact of disc dispersal, and find that the currently available sample sizes ($\sim 30$ discs at 5 Myr) introduce stochastic oscillations in the slopes evolution, which dominate over the physical signatures. Increasing the sample size could mitigate this issue: $\sim 140$ discs at 5 Myr, corresponding to the complete Upper Sco sample, would give small enough error bars to use the evolution of the slopes as a proxy for the driving mechanism of disc evolution. Finally, we discuss how the observational claim of steepening slopes necessarily leads to an initially steeper $M_d - M_*$ correlation with respect to $\dot M - M_*$.

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