标题： 从R136星团最近喷射出的OB高速星的起源 显示英文标题

标题： The origin of the most recently ejected OB runaway star from the R136 cluster

摘要： $\sim 60\,000$太阳质量（\MSun ）的星团 R136（NGC~2070）位于大麦哲伦星云中的蜘蛛星云中，是至少 55 颗大质量恒星（$M \apgt 10$ \MSun ）的宿主，这些恒星以投影速度$\gteq 27.5$km/s\cite{2024Natur.634..809S}远离星团。 这种逃逸恒星的高速度的起源自20世纪60年代以来一直存在争议，可能是由于动力学抛射\citep{1961BAN....15..265B,1961BAN....15..291B}或超新星爆炸\citep{1983ApJ...267..322H}引起的。由于盖亚卫星的卓越精度，我们现在可以追溯最近被抛射的双星系统Mel 34，将其回溯到R136的核心，并重建52000年前导致其从R136中移除的事件，即我们确定了其动力学相互作用和抛射历史。我们发现这次抛射需要由五颗恒星参与，其中包括由紧致大质量双星Mel~39围绕着VFTS~590恒星组成的三体系统，以及双星系统Mel~34。五颗恒星的参与是出乎意料的，因为逃逸恒星不期望来源于三体相互作用\cite{2011Sci...334.1380F}。散射中的牛顿动力学的确定性使我们能够重建抛射Mel~34的相遇。然后我们预测Mel~39是一对双星，拥有一个80\Msun 的伴星，该伴星在与Mel~34相同的平面上围绕其运行，以$\sim 1^\circ$的速度逃逸出星团，速度为$\sim 64$km/s。 五颗恒星将在接下来的5 Myr内在距离其诞生地（R 136）$\sim 180$光年到$\sim 332$光年的范围内发生超新星爆炸。然而，由此产生的黑洞双星预计不会在哈勃时间内合并。 显示英文摘要

摘要： The $\sim 60\,000$ solar-mass (\MSun) star-cluster R136 (NGC~2070) in the Tarantula Nebula in the Large Magellanic Cloud is the host of at least 55 massive stars ($M \apgt 10$\,\MSun) which move away from the cluster at projected velocities $\gteq 27.5$\,km/s \cite{2024Natur.634..809S}. The origin of the high velocities of such runaway stars have been debated since the 1960s, resulting either from dynamical ejections \citep{1961BAN....15..265B,1961BAN....15..291B} or from supernova explosions \citep{1983ApJ...267..322H}. Due to the Gaia satellite's outstanding precision, we can now retrace the most recently ejected binary star, Mel 34, back to the center of R136 and reconstruct the events that 52\,000 years ago let to its removal from R136, i.e., we establish its dynamical interaction and ejection history. We find that this ejection requires the participation of 5 stars in a strong interaction between a triple composed of the tight massive binary Mel~39 orbited by the star VFTS~590, and the binary star Mel~34. The participation of 5 stars is unexpected because runaway stars were not expected to result from triple interactions \cite{2011Sci...334.1380F}. The deterministic nature of the Newtonian dynamics in the scattering enables us to reconstruct the encounter that ejected Mel~34. We then predict that Mel~39 is a binary star with an 80\,\Msun\, companion star that orbits within $\sim 1^\circ$ in the same plane as Mel~34, and escapes the cluster with a velocity of $\sim 64$\,km/s. The five stars will undergo supernova explosions in the coming 5\,Myr at a distance of $\sim 180$\,pc to $\sim 332$\,pc from their birth location (R\,136). The resulting black hole binaries, however, are not expected to merge within a Hubble time.