Are debris discs self-stirred?
Are debris discs self-stirred?
复制标题
碎片盘是自搅拌的吗？
DOI：
10.1111/j.1365-2966.2010.16528.x
复制
发表时间：
2010
影响因子：
4.8
通讯作者：
M. Wyatt
中科院分区：
文献类型：
--
作者：
Grant M. Kennedy;M. Wyatt
本文的目的是考虑的证据表明，碎片盘是自搅拌的冥王星大小的物体的形成。本文提出了一个自搅拌尘埃的半解析模型，并应用于A星的统计。我们发现，5000万年前的A星的分数过剩之间没有显著的统计差异，因此专注于再现广泛的趋势，怀亚特等人（2007 b）的预搅拌模型没有预测的恒星分数的“上升和下降”。利用星群模型，我们发现，半径分布N（r）/r0.8在15- 120 AU之间，宽度dr = r=2的小行星带的自搅动模型可以再现这一统计和趋势。彗星必须有这个15 AU的最小半径，以显示在磁盘分数的峰值，而不是单调下降。然而，峰值在观测中的边缘意义意味着具有较小最小半径的模型也正式拟合数据。具有固定内半径和/或外半径的扩展盘的种群不符合统计数据，主要是由于随着搅拌在盘中进一步移动而缓慢的70米进化。这一结论，即碎片盘是狭窄的带而不是扩展的盘，是独立的24米趋势的年轻A星的意义。虽然上升和下降是自然解释的自搅拌，我们表明，统计数据也可以复制与模型中，磁盘被附近的偏心行星的长期扰动搅拌。详细的成像，可以揭示个别系统中的扭曲，尖锐的边缘和偏移，是消除搅拌的最佳方法。
This paper aims to consider the evidence that debris disks are self-stirred by the formation of Pluto-size objects. A semi-analytical model for the dust produced during self-stirring is developed and applied to the statistics for A stars. We show that there is no significant statistical difference between fractional excesses of A-stars .50Myr old, and therefore focus on reproducing the broad trends, the “rise and fall” of the fraction of stars with excesses that the pre-stirred model of Wyatt et al. (2007b) does not predict. Using a population model, we find that the statistics and trends can be reproduced with a self-stirring model of planetesimal belts with radius distribution N(r) / r 0.8 between 15–120AU, with width dr = r=2. Disks must have this 15AU minimum radius in order to show a peak in disk fraction, rather than a monotonic decline. However, the marginal significance of the peak in the observations means that models with smaller minimum radii also formally fit the data. Populations of extended disks with fixed inner and/or outer radii fail to fit the statistics, due mainly to the slow 70�m evolution as stirring moves further out in the disk. This conclusion, that debris disks are narrow belts rather than extended disks, is independent of the significance of 24�m trends for young A-stars. Although the rise and fall is naturally explained by self-stirring, we show that the statistics can also be reproduced with a model in which disks are stirred by secular perturbations from a nearby eccentric planet. Detailed imaging, which can reveal warps, sharp edges, and offsets in individual systems is the best way to characterise the stirring
灾难性小天体碰撞的全面数值模拟
影响因子：
3.2
作者：
Leinhardt Z
通讯作者：
Leinhardt Z
影响因子：
3.2
作者：
V. Mannings;A. Boss;S. Russell
通讯作者：
V. Mannings;A. Boss;S. Russell