发表机构
Columbia University; Massachusetts Institute of Technology; Flatiron Institute（哥伦比亚大学; 麻省理工学院; 平顿研究所）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
通过三维广义相对论磁流体动力学模拟，发现磁化坍缩星形成的黑洞可获得10^2--10^3 km/s的强诞生速度，影响黑洞保留与双星演化。
AI 中文摘要
非对称恒星爆炸通过线性动量守恒向其致密残骸施加冲量，即诞生速度。由于更大的质量吸积，黑洞（BH）的诞生速度通常被认为弱于中子星的速度，并且由于孤立黑洞在电磁上很暗，观测上更难约束。利用持续时间长达约30秒的三维广义相对论磁流体动力学模拟，我们表明，由快速旋转的大质量恒星（坍缩星）坍缩形成的、贯穿强大规模磁场黑洞可以获得10^2--10^3 km/s的大诞生速度。非对称电磁外流、磁通爆发和非球形抛射物的引力牵引塑造了速度大小，它们的相对贡献取决于前身星结构、磁通历史和黑洞自转。更快自转的黑洞受到更强、更接近自转轴对齐的速度，主要通过非对称喷流驱动抛射物的引力牵引。延迟过渡到磁 arrested 状态产生更非对称的外流，并能产生更强的反冲。因为我们的模型中所需的大规模磁通也是相对论性伽马射线暴喷流及其相关的高能喷流驱动超新星的关键成分，诞生速度可能是磁化坍缩星的自然结果。这样的速度可能显著改变致密恒星环境中的黑洞保留、双星生存、自转轨道失准，以及磁化坍缩星在产生对不稳定质量间隙内高自转黑洞方面的可行性。
英文摘要
Asymmetric stellar explosions impart an impulse, or natal kick, to their compact remnants by linear momentum conservation. Black hole (BH) natal kicks are often assumed to be weaker than neutron star kicks because of greater mass accretion, and they are harder to constrain observationally because isolated BHs are electromagnetically faint. Using 3D general-relativistic magnetohydrodynamic simulations lasting up to ~30 s, we show that BHs formed from the collapse of rapidly rotating massive stars (collapsars) threaded by strong large-scale magnetic fields can acquire large natal kicks 10^2--10^3 km/s. Asymmetric electromagnetic outflows, magnetic-flux eruptions, and the gravitational pull of aspherical ejecta shape the kick magnitude, and their relative contributions depend on the progenitor structure, magnetic-flux history, and BH spin. More rapidly spinning BHs receive stronger, more nearly spin-aligned kicks, primarily through the gravitational pull of asymmetric jet-driven ejecta. Delayed transitions to the magnetically arrested state produce more asymmetric outflows and can generate even stronger recoils. Because the large-scale magnetic flux required in our models is also a key ingredient of relativistic gamma-ray burst jets and their associated energetic, jet-driven supernovae, natal kicks may be a natural consequence of magnetized collapsars. Such kicks could substantially alter BH retention in dense stellar environments, binary survival, spin-orbit misalignment, and the viability of magnetized collapsars in producing highly spinning BHs within the pair-instability mass gap.
CommentsSubmitted to ApJ. 39 pages, 15 figures, 4 tables. Comments welcome
