标题： 脉冲星双星的偏心合并 显示英文标题

标题： Eccentric mergers of binary Proca stars

摘要： 我们对等质量旋转的$\bar m=1$ Proca 星进行了数值相对论研究，重点研究它们的引力波（GW）辐射。 通过系统地改变关键的二进制参数，例如决定轨道角动量的初始轨道助推，以及星体之间的相对相位，我们研究了 Proca 场的内部相位结构如何影响合并动力学和辐射的 GW 特性。 我们的模拟表明，相对相位对合并后的演化有决定性影响，导致伴随瞬时 Proca 残余物的快速黑洞形成，或者形成超质量的$\bar m=1$ Proca 星，甚至出现动态不稳定的旋转$\bar m=2$ Proca 星。 在某些条件下，GW 信号表现出传统黑洞合并中不存在的显著奇数模式（例如$\ell=m=3$模式），这可能作为这些奇异物体的独特特征。 我们的发现为玻色子星合并的表观现象学以及超轻玻色子场的潜在天体物理作用提供了新的见解。 显示英文摘要

摘要： We present a numerical relativity study of eccentric mergers of equal-mass rotating $\bar m=1$ Proca stars, focusing on their gravitational-wave (GW) emission. By systematically varying key binary parameters, such as the initial orbital boost, which determines the orbital angular momentum, and the relative phase between the stars, we examine how the internal phase structure of the Proca field influences the merger dynamics and the properties of the emitted GWs. Our simulations demonstrate that the relative phase has paramount impact on the post-merger evolution, resulting in prompt black hole formation accompanied by a transient Proca remnant, the formation of a hypermassive $\bar m=1$ Proca star or even the emergence of a dynamically-unstable spinning $\bar m=2$ Proca star. Under certain conditions, the GW signal exhibits significant odd-modes (e.g., the $\ell=m=3$ mode) that are absent in conventional black hole mergers, potentially serving as unique signatures of these exotic objects. Our findings offer new insights into the phenomenology of bosonic star mergers and the potential astrophysical role of ultralight bosonic fields.