论文标题
GW Orionis：带有翘曲磁盘和撕裂的环作为磁盘流体动力学基准的三重序列三倍
GW Orionis: A pre-main-sequence triple with a warped disk and a torn-apart ring as benchmark for disk hydrodynamics
论文作者
论文摘要
了解身体如何相互相互作用以及与磁盘材料相互作用，这是了解恒星系统和行星系统的结构的关键。虽然可以通过简单的重力来描述点源之间的相互作用，但与磁盘材料的相互作用需要进一步了解气体粘度和灰尘微物理学，这些知识在模拟磁盘体相互作用时需要包括在内。序列序列多个系统为我们提供了一个独特的实验室，以校准基本参数，例如粘度和测试可能塑造原始磁盘结构的流体动力学过程的理论，并影响这些磁盘形成的行星种群。在本文中，我简要回顾了我们对一个特别有趣的T Tauri Triple Star系统GW Orionis的了解，该系统有可能用作水动力学研究的罗塞塔石。长期干涉和径向速度监测，GW Orionis中恒星的3维轨道和质量受到约束。同样，强扭曲的磁盘的3维几何形状已基于高角度分辨率的热灰尘发射和散射光成像而紧密地构成。我们可能在GW Ori中看到的磁盘效果构成了将磁盘材料转移到高度倾斜或逆行轨道上的重要新机制，即使与恒星非常宽。同时，观察到的撕裂环似乎足够大，并且可能足够稳定，可以使行星形成，并有可能在高度倾斜的长期轨道上产生尚未发现的环形行星。
Understanding how bodies interact with each other and with disk material holds the key to understanding the architecture of stellar systems and of planetary systems. While the interactions between point sources can be described by simple gravity, interactions with disk material require further knowledge about the gas viscosity and dust microphysics that needs to be included when simulating disk-body interactions. Pre-main-sequence multiple systems provide us with a unique laboratory to calibrate fundamental parameters such as the viscosity and to test theories of hydrodynamic processes that might shape protoplanetary disk structure and affect the planet populations forming from these disks. In this article I briefly review our knowledge about a particularly intriguing T Tauri triple star system, GW Orionis, that has the potential to serve as a rosetta stone for hydrodynamic studies. The 3-dimensional orbits and masses of the stars in GW Orionis have been constrained by long-term interferometric and radial velocity monitoring. Also, the 3-dimensional geometry of the strongly distorted disk has been tightly contrained based on high-angular resolution thermal dust emission and scattered-light imaging. The disk-tearing effect that we might witness in GW Ori in action constitutes an important new mechanism for moving disk material onto highly oblique or retrograde orbits, even at very wide separations from the star. At the same time, the observed torn ring seems sufficiently massive, and might be sufficiently stable, for planet formation to occur, potentially giving rise to an yet-undiscovered population of circum-multiple planets on highly oblique, long-period orbits.
