Modelling circumbinary protoplanetary disks I. Fluid simulations of the Kepler-16 and 34 systems
Modelling circumbinary protoplanetary disks I. Fluid simulations of the Kepler-16 and 34 systems
复制标题
环双星原行星盘建模 I. Kepler-16 和 34 系统的流体模拟
DOI：
10.1051/0004-6361/201526295
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发表时间：
2015
影响因子：
6.5
通讯作者：
Lines S
中科院分区：
文献类型：
--
作者：
Lines S
开普勒任务发现了一些环绕双星的行星，这些行星的轨道接近（ap< 1.1 Au）恒星双星，这引发了一个问题，即这些行星是如何形成的，因为双星对圆盘产生了强烈的引力扰动。气体成分的circumbinary protoplanetary磁盘扰动以类似的方式固体，占主导地位的对应物，虽然磁盘偏心率起源的机制不同。AimsThis是第一个工作的一系列，旨在探讨行星形成的条件circumbinary protoplanetary disks.MethodsWe提出了一些流体动力学模拟，探讨两个观测到的双星系统周围的气体盘的响应：开普勒-16和开普勒-34我们探测的重要性盘的粘度，纵横比，内边界条件，初始表面密度梯度，和自引力的动力学演化的磁盘，以及其准稳态profile.ResultsWe发现有一个强烈的影响的二进制类型的平均磁盘偏心率，e d，导致toe d= 0.02 − 0.08的开普勒-16和dee d= 0.10 − 0.15的开普勒-34。α-粘性的值对盘的影响很小，但我们发现由于波的传播效应，盘的平均偏心率随着纵横比的增加而显著增加。内边界条件的选择对圆盘的面密度和偏心率影响不大。我们的主要发现是，包括磁盘的自引力对磁盘的质量小于12.5倍的最小质量太阳星云的演化或最终状态的影响很小。这一发现与自引力相关的结果，在环主磁盘，它的列入被认为是一个重要的因素，在描述磁盘的演变。
ContextTheKeplermission’s discovery of a number of circumbinary planets orbiting close (ap< 1.1 au) to the stellar binary raises questions as to how these planets could have formed given the intense gravitational perturbations the dual stars impart on the disk. The gas component of circumbinary protoplanetary disks is perturbed in a similar manner to the solid, planetesimal dominated counterpart, although the mechanism by which disk eccentricity originates differs.AimsThis is the first work of a series that aims to investigate the conditions for planet formation in circumbinary protoplanetary disks.MethodsWe present a number of hydrodynamical simulations that explore the response of gas disks around two observed binary systems: Kepler-16 and Kepler-34. We probe the importance of disk viscosity, aspect-ratio, inner boundary condition, initial surface density gradient, and self-gravity on the dynamical evolution of the disk, as well as its quasi-steady-state profile.ResultsWe find there is a strong influence of binary type on the mean disk eccentricity,e̅d, leading toe̅d= 0.02 − 0.08 for Kepler-16 ande̅d= 0.10 − 0.15 in Kepler-34. The value ofα-viscosity has little influence on the disk, but we find a strong increase in mean disk eccentricity with increasing aspect-ratio due to wave propagation effects. The choice of inner boundary condition only has a small effect on the surface density and eccentricity of the disk. Our primary finding is that including disk self-gravity has little impact on the evolution or final state of the disk for disks with masses less than 12.5 times that of the minimum-mass solar nebula. This finding contrasts with the results of self-gravity relevance in circumprimary disks, where its inclusion is found to be an important factor in describing the disk evolution.