论文标题
行星驱动螺旋中的灰尘动态
Dust dynamics in planet-driven spirals
论文作者
论文摘要
语境。众所周知，原月经磁盘可容纳在散射光，阿尔玛连续体以及CO气体发射和气体动力学中观察到的螺旋形特征。但是，气体和灰尘中的螺旋是否痕迹相同的形态是未知的。 目标。我们研究灰尘螺旋的形态和振幅是Stokes数量的功能以及导致气螺旋差异的潜在机制。然后，我们构建了一个模型，以将从气体中的开普勒旋转到气体和灰尘的表面密度扰动。 方法。我们将FARGO-3D与尘埃实施一起使用数值研究螺旋，然后使用半分析模型来解释结果。在观察数据上测试了该模型，以根据连续数据预测气体动力学中螺旋的扰动。 结果。我们发现气体和灰尘之间的螺旋螺旋角没有显着差异。灰尘螺旋的振幅随着stokes数量（ST）的降低，并且随着灰尘从气体与气体解耦时，典型的ST> 0.1开始褪色。半分析模型在气体的灰尘表面密度中提供了准确而快速的表示。我们在TW Hya速度残留图中发现了一个螺旋，从未见过，这是垂直速度的特征，并且在连续缝隙处有扭结，为99 AU的行星提供了有力的证据。 结论。我们构建了一个模型，该模型估算了螺旋形中灰尘的基本动力学，该模型可以用作螺旋的行星起源的证明，并且可以作为磁盘中Stokes数字的探测器。
Context. Protoplanetary disks are known to host spiral features that are observed in scattered light, ALMA continuum and more recently in CO gas emission and gas dynamics. It is however unknown if spirals in gas and dust trace the same morphology. Aims. We study the morphology and amplitude of dusty spirals as function of Stokes number and the underlying mechanisms causing a difference from gas spirals. We then construct a model to relate the deviation from Keplerian rotation in the gas to a perturbation in surface density of gas and dust. Methods. We use FARGO-3D with dust implementation to numerically study the spirals, after which the results are interpreted using a semi-analytical model. This model is tested on observational data to predict the perturbation of the spiral in gas dynamics based on the continuum data. Results. We find that the pitch angle of a spiral does not differ significantly between gas and dust. The amplitude of the dust spiral decreases with Stokes number (St) and starts to fade out at a typical St > 0.1 as the dust becomes decoupled from the gas. The semianalytical model provides an accurate and fast representation of the spiral in surface density of the dust from the gas. We find a spiral in the TW Hya velocity residual map, never seen before, which is a feature in the vertical velocity and has a kink at the continuum gap, yielding strong evidence for a planet at 99 au. Conclusions. We built a model that gives an estimate of the underlying dynamics of dust in a spiral, which can serve as a proof of planetary origin of spirals and can be a probe for the Stokes number in the disk.
