The crucial role of higher order multiplicity in wide binary formation: a case study using the β-Pictoris moving group
The crucial role of higher order multiplicity in wide binary formation: a case study using the β-Pictoris moving group
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高阶多重性在宽二元形成中的关键作用：使用 β-Pictoris 移动群的案例研究
DOI：
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发表时间：
2016
期刊：
影响因子：
--
通讯作者：
A. Bayo
中科院分区：
文献类型：
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作者：
P. Elliott;A. Bayo
很难解释“就地”形成非常宽的双星的原因，因为它们的物理分离超出了崩塌的云核的典型大小(约5000-10000美元)。在这里，我们研究了这种系统的形成过程。我们计算了β-Pictoris运动群(BPMG)中伴星的多重数分数(MF)、伴星分数(CSF)和物理间隔分布等布居统计量。我们比较了以前在年轻和老年地区的多重性研究，结果表明，原始多重性程度高的年轻种群的动态演化可以导致类似于田间种群的过程分离分布。外部分量的演化归因于更高阶(三重)系统的动力学展开；其自然结果是宽双星的形成。我们发现，我们强烈倾向于宽系统包含三个或更多组件($>；$1000 Au：11/14，10,000 Au：6/7)。我们认为，在年轻的移动群体中发现的大多数宽双星都是原始的。在假设我们银河系内的恒星群具有统计上相似的原始多重性的情况下，我们可以推断，该场中宽双星的稀少是动力学演化的结果。
The "in-situ" formation of very wide binaries is hard to explain as their physical separations are beyond the typical size of a collapsing cloud core ($\approx$5000-10,000 au). Here we investigate the formation process of such systems. We compute population statistics such as the multiplicity fraction (MF), companion-star fraction (CSF) and physical separation distribution of companions in the $\beta$-Pictoris moving group (BPMG). We compare previous multiplicity studies in younger and older regions and show that the dynamic evolution of a young population with a high degree of primordial multiplicity can lead to a processed separation distribution, similar to the field population. The evolution of outer components is attributed to the dynamical unfolding of higher-order (triple) systems; a natural consequence of which is the formation of wide binaries. We find a strong preference for wide systems to contain three or more components ($>$1000 au: 11 / 14, 10,000 au: 6 / 7). We argue that the majority of wide binaries identified in young moving groups are primordial. Under the assumption that stellar populations, within our galaxy, have statistically similar primordial multiplicity, we can infer that the paucity of wide binaries in the field is the result of dynamical evolution.
DOI：
10.1088/0004-637x/777/2/160
发表时间：
2013-09
期刊：
The Astrophysical Journal
影响因子：
--
作者：
B. Biller;Michael C. Liu;Z. Wahhaj;E. Nielsen;Thomas L. Hayward;J. Males;A. Skemer;L. Close;M. Chun;C. Ftaclas;F. Clarke;N. Thatte;E. Shkolnik;I. N. Reid;M. Hartung;A. Boss;D. Lin;S. Alencar;E. M. de Gouveia Dal Pino;J. Gregorio-Hetem;D. Toomey
通讯作者：
B. Biller;Michael C. Liu;Z. Wahhaj;E. Nielsen;Thomas L. Hayward;J. Males;A. Skemer;L. Close;M. Chun;C. Ftaclas;F. Clarke;N. Thatte;E. Shkolnik;I. N. Reid;M. Hartung;A. Boss;D. Lin;S. Alencar;E. M. de Gouveia Dal Pino;J. Gregorio-Hetem;D. Toomey
影响因子：
3.2
作者：
V. Mannings;A. Boss;S. Russell
通讯作者：
V. Mannings;A. Boss;S. Russell
影响因子：
6.5
作者：
Baraffe, Isabelle;Homeier, Derek;Chabrier, Gilles
通讯作者：
Chabrier, Gilles