论文标题
嵌入原星磁盘中的低质量行星诱导的气流和间隙形成$ \ rm i $。稳态模型
Dust ring and gap formation by gas flow induced by low-mass planets embedded in protoplanetary disks $\rm I$. Steady-state model
论文作者
论文摘要
最近的高空间分辨率观察结果揭示了诸如环和缝隙之类的原行星磁盘中的灰尘子结构，它们并不总是与气体相关。由于低质量引起的径向气流，因此非气流间隙开放的行星可能会影响灰尘的径向漂移，因此它可能在磁盘中形成这些灰尘子结构。我们研究了低质量行星诱导的气流的潜力，以雕刻灰尘曲线中的环和间隙。我们首先执行三维流体动力模拟，该模拟可以解决局部气体流过的行星。然后，我们计算受行星诱导的气流影响的尘埃轨迹。最后，我们通过将行星诱导的气流的影响纳入一维灰尘对流扩散模型来计算稳态尘埃表面密度。气体向行星轨道外部的流出抑制了灰尘的径向漂移，导致灰尘积聚（灰尘环）。朝向行星轨道内部的流出会增强灰尘的内向漂移，从而导致灰尘围绕行星轨道（灰尘缝隙）耗尽。在微弱的湍流下（$α_ {\ rm diff} \ LISSSIM10^{ - 4} $，其中$α_ {\ rm diff} $是湍流强度参数），由$ \ gtrsim1 \ gtrsim1 \，m _ _ _ {gtrates gentrates ristate y generation and turtate tust under（graties and generation）诱发的气流（gtrsim1 （$ \ Lessim1 $ cm）径向范围为$ \ sim1 \ text { - } 10 $乘以行星轨道周围的气体尺度，而不会产生气体间隙和压力凸起。低质量，非气体间隙开放的行星引起的气流可以被认为是磁盘中观察到的尘埃子结构的可能起源。我们的结果可能有助于解释其灰尘子结构与气体无关的磁盘。
Recent high-spatial-resolution observations have revealed dust substructures in protoplanetary disks such as rings and gaps, which do not always correlate with gas. Because radial gas flow induced by low-mass, non-gas-gap-opening planets could affect the radial drift of dust, it potentially forms these dust substructures in disks. We investigate the potential of gas flow induced by low-mass planets to sculpt the rings and gaps in the dust profiles. We first perform three-dimensional hydrodynamical simulations, which resolve the local gas flow past a planet. We then calculate the trajectories of dust influenced by the planet-induced gas flow. Finally, we compute the steady-state dust surface density by incorporating the influences of the planet-induced gas flow into a one-dimensional dust advection-diffusion model. The outflow of the gas toward the outside of the planetary orbit inhibits the radial drift of dust, leading to dust accumulation (the dust ring). The outflow toward the inside of the planetary orbit enhances the inward drift of dust, causing dust depletion around the planetary orbit (the dust gap). Under weak turbulence ($α_{\rm diff}\lesssim10^{-4}$, where $α_{\rm diff}$ is the turbulence strength parameter), the gas flow induced by the planet with $\gtrsim1\,M_{\oplus}$ (Earth mass) generates the dust ring and gap in the distribution of small dust grains ($\lesssim1$ cm) with the radial extent of $\sim1\text{--}10$ times gas scale height around the planetary orbit without creating a gas gap and pressure bump. The gas flow induced by low-mass, non-gas-gap-opening planets can be considered a possible origin of the observed dust substructures in disks. Our results may be helpful to explain the disks whose dust substructures were found not to correlate with those of the gas.
