论文标题
估计行星在怪异轨道中开放的间隙的深度
Estimating the depth of gaps opened by planets in eccentric orbit
论文作者
论文摘要
行星可以在原球盘的表面密度中雕刻间隙。这些间隙的形成可以减少作用在行星上的旋转扭矩。此外，由于可能会捕获间隙边缘的灰尘和卵石，因此间隙会停止固体的积聚到行星上。这种尘埃的积累可以解释使用高分辨率干涉法观察到的环状灰尘结构的起源。在这项工作中，我们为行星在怪异轨道上清除的差距的深度提供了经验缩放关系，这是行星与星级质量比$ q $，盘宽高比$ h $，shakura-sunyaev粘度参数$α$和行星偏心元素$ e $ e $ e $。我们使用启发式方法构建缩放关系：我们基于使用2D流体动力学模拟的脉冲近似校准玩具模型。缩放缩放重现了中等偏心率的间隙深度（$ e \ leq 4h $），当间隙外部和内部的表面密度对比度为$ \ leq 10^{2} $时。我们的框架可以用作更复杂的模型的基础，旨在预测偏心行星的径向间隙轮廓。
Planets can carve gaps in the surface density of protoplanetary discs. The formation of these gaps can reduce the corotation torques acting on the planets. In addition, gaps can halt the accretion of solids onto the planets as dust and pebbles can be trapped at the edge of the gap. This accumulation of dust could explain the origin of the ring-like dust structures observed using high-resolution interferometry. In this work we provide an empirical scaling relation for the depth of the gap cleared by a planet on an eccentric orbit as a function of the planet-to-star mass ratio $q$, the disc aspect ratio $h$, Shakura-Sunyaev viscosity parameter $α$, and planetary eccentricity $e$. We construct the scaling relation using a heuristic approach: we calibrate a toy model based on the impulse approximation with 2D hydrodynamical simulations. The scaling reproduces the gap depth for moderate eccentricities ($e\leq 4h$) and when the surface density contrast outside and inside the gap is $\leq 10^{2}$. Our framework can be used as the basis of more sophisticated models aiming to predict the radial gap profile for eccentric planets.
