AI 中文总结
研究通过拟合分子示踪剂速度旋转曲线确定原行星盘质量等参数，扩展动力学方法用于有吸收特征的源，强调束展宽校正，通过自举重采样估计不确定性，还探讨了盘稳定性与毫米尘埃螺旋形态的联系。
AI 中文摘要
确定原行星盘的总质量对于了解行星形成的物质可用性至关重要，但精确测量盘质量具有挑战性。研究气体动力学是精确表征盘质量的有力且与示踪剂无关的方法。通过用包含盘热分层和自引力的精确模型拟合不同分子示踪剂的速度旋转曲线，我们确定了HD 97048和WaOph 6周围盘的恒星质量、盘质量和尺度半径，并测量了相应的气尘比和盘星质量比。我们有效地扩展了动力学方法以表征具有吸收特征的嵌入源，证明了对曲线进行束展宽校正的重要性，通过对两个盘的几何结构和二维热结构进行自举重采样提供了最佳拟合参数系统不确定性的综合估计，最后通过比较所有动态称重盘的Toomre参数研究了盘稳定性与毫米连续谱发射中螺旋形态出现之间的联系，表明有毫米尘埃螺旋的盘的Q值系统地更低。
英文摘要
Constraining the total mass of protoplanetary disks is crucial to determine the availability of material for planet formation. Yet, providing accurate and precise measurements of the disk mass is challenging. Investigating the gas dynamics is a powerful, tracer-independent method to precisely characterize disk masses. By fitting the velocity rotation curves of different molecular tracers with an accurate model including the disk thermal stratification and self-gravity, we constrain the stellar masses, disk masses, and scale radii for the disks around HD 97048 and WaOph 6. We obtain $M_\star=2.226 ^{+0.054}_{-0.049}\ M_\odot$, $M_\mathrm{d}=0.3 ^{+0.055}_{-0.061}\ M_\odot$ and $R_\mathrm{c}=172 ^{+24}_{-14}$ au for HD 97048, and $M_\star=0.956\ ^{+0.006}_{-0.006}\ M_\odot$, $M_\mathrm{d}=0.21 ^{+0.045}_{-0.038}\ M_\odot$ and $R_\mathrm{c}=647 ^{+193}_{-155}$ au for WaOph 6. We also measure the corresponding gas-to-dust and disk-to-star mass ratios. We efficiently extend the dynamical method to characterize embedded sources exhibiting features of absorption, for which a careful analysis is required to avoid biases in the retrieved velocity profiles. We prove the importance of including a beam smearing correction to the curves: if not, this observational effect can systematically bias the velocity profiles, altering the disk mass estimates up to $\sim45\%$. We provide comprehensive estimates of the systematic uncertainties on the best-fit parameters by bootstrapping over both the retrieved geometry and 2D thermal structure of the two disks: the overall uncertainty on the disk masses is $\sim20\%$. Finally, we investigate the connection between disk stability and the appearance of spiral morphologies in the mm continuum emission, by comparing the Toomre parameter of all dynamically weighed disks to date, showing that disks with mm-dust spirals have systematically lower values of Q.
