发表机构
Univ. Grenoble Alpes, CNRS, IPAG; Instituto de Astronomía Teórica y Experimental (IATE), UNC-CONICET; Instituto de Astrofísica, Pontificia Universidad Católica de Chile; School of Physics & Astronomy, University of Birmingham（格勒诺布尔阿尔卑斯大学; 理论与实验天文学研究所; 智利天主教大学天体物理研究所; 伯明翰大学物理与天文学院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过N体模拟结合行星迁移方案，探究双星属性与迁移场景对环双行星稳定性的影响，发现双星质量比、偏心率及迁移时标是关键因素，为识别宜居双星系统提供了依据。
AI 中文摘要
在迄今发现的数千颗系外行星中，只有极小一部分被归类为环双行星，若考虑低质量行星，这一数量可忽略不计。这种稀有性部分源于观测偏差，也源于双星系统中极具挑战性的动力学环境，该环境会阻碍行星轨道的长期稳定性。因此，研究使稳定环双行星形成并存活的条件，尤其是在低质量范围内的条件，至关重要。为此，我们开展了N体模拟并结合行星迁移方案，研究原行星盘中两颗10倍地球质量环双行星的形成后动力学。基于1000余次模拟，我们发现向内迁移有时可通过与双星的共振捕获而暂停。与某些此前的纯N体研究不同，这些构型似乎能在长期内保持稳定。我们进一步发现，双星质量比$q_B$和偏心率$e_B$强烈影响多行星系统的稳定性。在所探索的参数空间内，部分区域支持长期稳定，而其他区域则高度不稳定。这些稳定区域还对迁移时标敏感，因此也对盘属性和行星质量敏感。最后，我们的模拟表明，两颗行星在共同迁移时进入共振的系统更可能形成稳定的多行星构型，尤其在高偏心率双星周围。这些结果为识别最有可能拥有多颗低质量环双行星的双星系统迈出了第一步。
英文摘要
Among the thousands of exoplanets detected to date, only a very small fraction are classified as circumbinary planets, and this number becomes negligible when considering low-mass planets. This rarity may partly result from observational biases, but also from the challenging dynamical environment of binary systems, which can prevent the long-term stability of planetary orbits. It is therefore essential to investigate the conditions that enable the formation and survival of stable circumbinary planets, particularly in the low-mass regime. To this end, we performed N-body simulations coupled with a planet migration prescription to study the post-formation dynamics of two 10 Earth-mass circumbinary planets in a protoplanetary disc. Based on more than 1,000 simulations, we find that inward migration can, in some cases, be halted through resonance capture with the binary. In contrast to some previous purely N-body studies, these configurations appear to remain stable over long timescales. We further find that the binary mass ratio $q_B$ and eccentricity $e_B$ strongly influence the stability of multi-planet systems. Within the explored parameter space, some regions support long-term stability, whereas others are highly unstable. These stability regions are also sensitive to the migration timescales, and therefore to disc properties and planetary masses. Finally, our simulations suggest that systems in which two planets enter resonance while migrating together are more likely to form stable multi-planet configurations, particularly around highly eccentric binaries. These results provide a first step toward identifying binary star systems that are most promising for hosting multiple low-mass circumbinary planets.
Comments19 pages, 15 figures. Accepted for publication in A&A
