Eccentric Modes in Disks with Pressure and Self-gravity
Eccentric Modes in Disks with Pressure and Self-gravity
复制标题
具有压力和自重力的圆盘中的偏心模式
DOI：
10.3847/1538-4357/ab010c
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发表时间：
2018
期刊：
影响因子：
--
通讯作者：
Y. Lithwick
中科院分区：
文献类型：
--
作者：
Wing;A. Dempsey;Y. Lithwick
恒星周围的吸积盘，或其他中心大质量天体，可以支持长期存在的，缓慢进动的m = 1扰动，其中流体运动接近开普勒，偏心率非零。我们研究这种“慢模式”的磁盘，受到压力和自重力。我们推导出一个二阶WKB色散关系，描述的动态相当准确，并表明，显然复杂的性质的各种模式可以理解在一个简单的方式与图形方法的帮助。数值求解了线性化的流体方程组，结果与理论一致。我们发现，当自引力是弱的（，其中Q是Toomre的参数和h是磁盘的纵横比），模式是压力占主导地位。但当自引力较强（）时，出现两种引力主导模式：一种是排列的椭圆模式，另一种是单臂螺旋模式。在原行星盘的背景下，我们建议，如果径向偏心率的轮廓可以测量，它可以用来确定总盘质量。
Accretion disks around stars, or other central massive bodies, can support long-lived, slowly precessing m = 1 disturbances in which the fluid motion is nearly Keplerian with non-zero eccentricity. We study such “slow modes” in disks that are subject to both pressure and self-gravity forces. We derive a second-order WKB dispersion relation that describes the dynamics quite accurately and show that the apparently complicated nature of the various modes can be understood in a simple way with the help of a graphical method. We also solve the linearized fluid equations numerically and show that the results agree with the theory. We find that when self-gravity is weak ( , where Q is Toomre’s parameter and h is the disk aspect ratio), the modes are pressure-dominated. But when self-gravity is strong ( ), two kinds of gravity-dominated modes appear: one is an aligned elliptical pattern and the other is a one-armed spiral. In the context of protoplanetary disks, we suggest that if the radial eccentricity profile can be measured, it could be used to determine the total disk mass.
二维偏心开普勒圆盘的非线性流体动力学演化：世俗理论的验证
DOI：
10.48550/arxiv.1603.02544
发表时间：
2016
期刊：
--
影响因子：
--
作者：
Barker A
通讯作者：
Barker A
DOI：
10.3847/1538-4357/aab15c
发表时间：
2017-12
期刊：
The Astrophysical Journal
影响因子：
--
作者：
C. Chan;J. Krolik;T. Piran
通讯作者：
C. Chan;J. Krolik;T. Piran