环双星行星系统中起源的自由漂浮行星的性质
On the properties of free floating planets originating in circumbinary planetary systems
AI总结：
本研究探讨了环双星系统中自由漂浮行星的形成与抛射机制，发现双星抛射与行星相互作用抛射在速度分布上存在显著差异，且大质量行星频率与束缚行星相似，为观测区分形成路径提供了理论预测。
摘要：
自由漂浮行星是最近发现的一类新行星。这些行星不在恒星系统内运行，而是在星系中过着游荡的生活。这类天体是如何形成的仍然是个谜。许多研究探索了形成此类天体的机制，但尚未提供能够区分不同形成机制的分布预测。在这项工作中，我们在环双星系统中形成这些天体，在这些系统中，行星很容易形成并通过与中心双星的相互作用被弹出。我们发现通过行星与行星相互作用弹出的行星与被双星弹出的行星之间存在显著差异。出现的主要差异在于超额速度的分布，双星以更快的速度弹出行星。这些差异应该在附近恒星形成区域的已知自由漂浮行星中是可观测的。我们预测，对这些区域中直接成像的自由漂浮行星进行定向观测，应该能够确定它们首选的形成路径，无论是在单星或多星系统中通过行星形成，还是通过类似于恒星形成的过程。此外，自由漂浮行星的质量分布可以为了解潜在的行星种群提供重要见解。我们发现，对于质量大于20 $\rm M_{\oplus}$ 的行星，其频率与那些保持束缚并在中心双星附近运行的行星相似。这种相似性使得微透镜巡天的质量分布能够与凌日和径向速度的质量分布进行有效且信息丰富的比较。最终，通过观测自由漂浮行星的速度弥散和质量分布，将有可能有效地与行星形成模型的预测进行比较，并进一步了解这些奇异世界的形成与演化。
英文摘要：
Free-floating planets are a new class of planets recently discovered. These planets don't orbit within stellar systems, instead living a nomadic life within the galaxy. How such objects formed remains elusive. Numerous works have explored mechanisms to form such objects, but have not yet provided predictions on their distributions that could differentiate between formation mechanisms. In this work we form these objects within circumbinary systems, where these planets are readily formed and ejected through interactions with the central binary stars. We find significant differences between planets ejected through planet-planet interactions and those by the binary stars. The main differences that arise are in the distributions of excess velocity, where binary stars eject planets with faster velocities. These differences should be observable amongst known free-floating planets in nearby star-forming regions. We predict that targeted observations of directly imaged free-floating planets in these regions should be able to determine their preferred formation pathway, either by planet formation in single or multiple stellar systems, or through processes akin to star formation. Additionally the mass distributions of free-floating planets can yield important insights into the underlying planet populations. We find that for planets more massive than 20 $\rm M_{\oplus}$, their frequencies are similar to those planets remaining bound and orbiting near the central binaries. This similarity allows for effective and informative comparisons between mass distributions from microlensing surveys, to those of transit and radial velocities. Ultimately, by observing the velocity dispersion and mass distribution of free-floating planets, it will be possible to effectively compare with predictions from planet formation models, and to further understand the formation and evolution of these exotic worlds.
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