自破坏螺旋波：吸积盘中螺旋波不稳定性的全球模拟
Self-Destructing Spiral Waves: Global Simulations of a Spiral Wave Instability in Accretion Disks
摘要：
我们提出的结果从一套三维全球流体动力学模拟表明，螺旋密度波传播在拱盘是不稳定的增长的参数不稳定，导致故障的流动成湍流。这种螺旋波不稳定性（SWI）是由惯性波或惯性-重力波与背景螺旋波之间的共振相互作用引起的。在线性制度的不稳定性的发展涉及的增长的一个广泛的频谱的惯性模式，增长率的顺序的轨道时间，并导致在一个非线性饱和状态，其中湍流速度扰动是一个类似的幅度所引起的螺旋波。湍流引起角动量输运和垂直混合，其速率局部取决于螺旋波的振幅（我们在参考模型中获得应力参数$α\sim 5 \times 10^{-4}$）。不稳定性被发现在广泛的磁盘模型，包括那些与等温或绝热状态方程，并在粘性磁盘中的无量纲运动粘度$ν\le 10^{-5}$。这种鲁棒性表明，不稳定性将应用于广泛的天体物理磁盘相关的现象，包括那些在密切的双星系统，行星嵌入原行星盘（包括木星在我们自己的太阳系）和FU猎户座爆发模型。需要进一步的工作，以确定不稳定性的性质，并评估其观测结果，在物理上更完整的磁盘模型比我们在本文中所考虑的。
英文摘要：
We present results from a suite of three-dimensional global hydrodynamic simulations which show that spiral density waves propagating in circumstellar disks are unstable to the growth of a parametric instability that leads to break-down of the flow into turbulence. This spiral wave instability (SWI) arises from a resonant interaction between pairs of inertial waves, or inertial-gravity waves, and the background spiral wave. The development of the instability in the linear regime involves the growth of a broad spectrum of inertial modes, with growth rates on the order of the orbital time, and results in a nonlinear saturated state in which turbulent velocity perturbations are of a similar magnitude to those induced by the spiral wave. The turbulence induces angular momentum transport, and vertical mixing, at a rate that depends locally on the amplitude of the spiral wave (we obtain a stress parameter $α\sim 5 \times 10^{-4}$ in our reference model). The instability is found to operate in a wide-range of disk models, including those with isothermal or adiabatic equations of state, and in viscous disks where the dimensionless kinematic viscosity $ν\le 10^{-5}$. This robustness suggests that the instability will have applications to a broad range of astrophysical disk-related phenomena, including those in close binary systems, planets embedded in protoplanetary disks (including Jupiter in our own Solar System) and FU Orionis outburst models. Further work is required to determine the nature of the instability, and to evaluate its observational consequences, in physically more complete disk models than we have considered in this paper.
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