Simulations of the Fomalhaut system within its local galactic environment
Simulations of the Fomalhaut system within its local galactic environment
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北落师门系统在其当地银河环境中的模拟
DOI：
10.1093/mnras/stx2456
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发表时间：
2017
影响因子：
4.8
通讯作者：
Izidoro, André
中科院分区：
文献类型：
--
作者：
Kaib, Nathan A.;White, Ethan B.;Izidoro, André
北落师门A是附近最受研究的恒星之一，已被发现拥有一个假定的行星物体和一个引人注目的偏心尘埃带。这一偏心尘埃带通常被解释为一颗或多颗行星的动力学特征，而不是直接探测到的。我们设计了一个新的辛积分算法来模拟北落师门A行星尘埃带的演化与其伴星的动力学演化，以确定这些伴星是否可能产生了尘埃带的形态。使用我们的数值模拟，我们发现北落总科A和B之间的近距离相遇是可以预期的，这两颗恒星在某个时间点经过对方至少400au以内的概率为∼25 / 。尽管这种相遇历史的结果千差万别，但这些近距离相遇几乎总是激发出北落科A尘埃带的偏心率，偶尔会产生与观测到的尘埃带非常相似的形态。根据这些结果，我们认为，与北落总科A的恒星伴星的近距离相遇应该被认为是解释其偏心带的一种合理的机制，特别是在没有检测到能够塑造该带形态的行星的情况下。更广泛地说，我们还可以从这项工作中得出结论，非常宽的双星通常会在它们所在的恒星碎片盘中产生不对称性。
Fomalhaut A is among the most well-studied nearby stars and has been discovered to possess a putative planetary object as well as a remarkable eccentric dust belt. This eccentric dust belt has often been interpreted as the dynamical signature of one or more planets that elude direct detection. However, the system also contains two other stellar companions residing ∼105au from Fomalhaut A. We have designed a new symplectic integration algorithm to model the evolution of Fomalhaut A's planetary dust belt in concert with the dynamical evolution of its stellar companions to determine if these companions are likely to have generated the dust belt's morphology. Using our numerical simulations, we find that close encounters between Fomalhaut A and B are expected, with an ∼25 per cent probability that the two stars have passed within at least 400 au of each other at some point. Although the outcomes of such encounter histories are extremely varied, these close encounters nearly always excite the eccentricity of Fomalhaut A's dust belt and occasionally yield morphologies very similar to the observed belt. With these results, we argue that close encounters with Fomalhaut A's stellar companions should be considered a plausible mechanism to explain its eccentric belt, especially in the absence of detected planets capable of sculpting the belt's morphology. More broadly, we can also conclude from this work that very wide binary stars may often generate asymmetries in the stellar debris discs they host.
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发现北落师门 C 碎片盘
DOI：
10.1093/mnrasl/slt168
发表时间：
2013
影响因子：
--
作者：
G. Kennedy;M. Wyatt;P. Kalas;G. Duchêne;B. Sibthorpe;J. Lestrade;B. Matthews;J. Greaves
通讯作者：
J. Greaves
1.3 毫米 ALMA 对北落师门碎片系统的观测
影响因子：
4.8
作者：
J. White;A. Boley;W. Dent;E. Ford;S. Corder
通讯作者：
S. Corder
DOI：
10.1086/301553
发表时间：
2000
期刊：
The Astronomical Journal
影响因子：
--
作者：
H. Levison;M. Duncan
通讯作者：
M. Duncan
DOI：
--
发表时间：
2013
期刊：
影响因子：
--
作者：
E. Mamajek;Jennifer Lynn Bartlett;A. Seifahrt;T. Henry;S. Dieterich;John C. Lurie;M. Kenworthy;W. Jao;A. Riedel;J. Subasavage;J. Winters;C. Finch;P. Ianna;J. Bean
通讯作者：
J. Bean
作为北落师门尘埃带结构起源的行星系统
影响因子：
64.8
作者：
P. Kalas;J. Graham;M. Clampin
通讯作者：
M. Clampin