We aim to observationally and statistically constrain the influence of flybys in the formation and evolution of debris disks. We compiled a sample of 254 debris disks with ages between 2 Myr and 8 Gyr that are either part of an association or isolated, drawing the binary and planetary companions of the systems mainly from the literature. Using the Gaia eDR3 astrometric data and radial velocities of our sample, as well as all the sources in a specific region of the sky, we reconstructed the relative linear motions in the last 5 Myr and made predictions for the next 2 Myr. Relating the Hill radius of each debris disk system and the closest distances reached by the two sources, we defined the flyby events in terms of position and time. We find that in the period between the last 5 Myrs and the next 2 Myrs, 90% of the analyzed systems have experienced at least a close flyby, while 7% of them have experienced flybys at distances greater than 0.5R Hill. In particular, 75% of them have experienced at least one past close encounter and 36% multiple past close encounters. From the sub-sample of resolved debris disk (41 out of 94), 80% of the analyzed systems experience at least an encounter within 0.8 pc. From the subsample of 10 debris disks with planets, half of these systems do show misalignments between disk and planet, stirring, or asymmetries. Systems with a misalignment between the planetary orbit and the disk do indeed experience at least one flyby event. In particular, when the planet orbits have a difference with the disk inclination higher than about 20 degree, as in the case of HD 38529, we find that multiple close encounters have taken place in the last 5 Myr, as theoretically predicted. The high incidence of encounters, particularly close encounters, experienced by the systems in the last 5 Myr suggests the fundamental impact of flybys on the evolution of debris disks.
Inclination Excitation of Solar System Debris Disk due to Stellar Flybys
大多数恒星形成于星团中，在星团中与其他恒星相对近距离的相遇是很常见的，并且可以在行星系的轨道结构上留下印记。在本文中，我们调查的倾斜激励的碎片盘粒子由于这样的恒星遭遇。我们推导出一个解析表达式，描述倾斜激发的恒星飞越是遥远的层次限制。然后，我们得到相应的粒子倾角分布在非分级制度使用一个大的合奏N体模拟的数值结果。对于遇到预期的参数，我们发现，磁盘粒子的散装倾角仍然很低。然而，一个独特的高倾角人口产生的天体碰撞粒子的最终近心距离以上$50$ AU。最大程度$i_t$的倾角分布规模与遇到$\sin(i_s)$的大质量恒星飞掠低入射速度的倾角。观测到的海王星外天体的倾角分布对我们太阳系的动力学历史产生了限制。例如，这些结果意味着太阳诞生星团的数密度$n$和太阳停留时间$τ$的乘积的上限，其形式为$nτ\lesssim8\times10^4$ Myr pc $^{-3}$。随着今后对外太阳系的观测调查，可以得出更强的限制。
Environmental interactions in Class II systems and their impact on the disk-planet architecture
Univ. Grenoble Alpes（格勒诺布尔阿尔卑斯大学）；CNRS（法国国家科学研究中心）；IPAG（格勒诺布尔行星与天体物理实验室）；University of Warwick（华威大学）；Tsinghua University（清华大学）；Monash University（莫纳什大学）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯玻尔研究所）
3I/ATLAS: In Search of the Witnesses to Its Voyage
Universidade da Coruña (UDC)（拉科鲁尼亚大学）；CIGUS CITIC, Centre for Information and Communications Technologies Research（信息与通信技术研究中心 CIGUS CITIC）；Institute of Science and Technology Austria (ISTA)（奥地利科学技术研究所）；Instituto de Astrofísica de Canarias（加那利天体物理研究所）；Universidad de La Laguna (ULL)（拉古纳大学）；Lund Observatory, Division of Astrophysics, Department of Physics, Lund University（隆德大学天文台）
A Kinematic History of Stellar Encounters with Beta Pictoris
Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心）；Universidad Complutense de Madrid（马德里康普顿斯大学）；Institute of Science and Technology Austria (ISTA)（奥地利科学技术研究所）；Lund University（隆德大学）；Instituto de Astrofísica de Canarias（加那利天体物理研究所）；Universidad de La Laguna (ULL)（拉各拉纳大学）
