中子星：形成、自旋和反冲
Neutron Stars: Formed, Spun and Kicked
摘要：
研究有中子星的恒星系统的主要目标之一是揭示祖先的物理性质，并了解中子星的自旋和出生踢是如何确定的。多年来，人们已经达成了共识，但最近，这种理解的一些基本要素受到了目前对一些双星系统的观测及其理论解释的挑战。在下文中，我们回顾了这些最新的发展，并强调它们是如何相互联系的;我们特别强调了理论解释的一些假设和警告，并检查了它们的有效性（例如，与未知的恒星径向速度或多维统计分析的细微差别有关）。新出现的图像并没有抹去我们早期的理解，相反，它拓宽了它，因为它揭示了中子星形成和演化的额外途径：中子星可能形成于大质量恒星Fe核的核塌缩和低质量恒星ONeMg核的电子捕获超新星的结束;分娩踢脚要求高（远远超过100 km/s），对于某些中子星和低（< 100 km/s），取决于形成过程;而自旋上升不仅可能通过罗奇瓣溢出发生，也可能通过风吸积或在共同包层演化过程中的超临界吸积阶段发生。
英文摘要：
One of the primary goals when studying stellar systems with neutron stars has been to reveal the physical properties of progenitors and understand how neutron star spins and birth kicks are determined. Over the years a consensus understanding had been developed, but recently some of the basic elements of this understanding are being challenged by current observations of some binary systems and their theoretical interpretation. In what follows we review such recent developments and highlight how they are interconnected; we particularly emphasize some of the assumptions and caveats of theoretical interpretations and examine their validity (e.g., in connection to the unknown radial velocities of pulsars or the nuances of multi-dimensional statistical analysis). The emerging picture does not erase our earlier understanding; instead it broadens it as it reveals additional pathways for neutron star formation and evolution: neutron stars probably form at the end of both core collapse of Fe cores of massive stars and electron-capture supernovae of ONeMg cores of lower-mass stars; birth kicks are required to be high (well in excess of 100 km/s) for some neutron stars and low (< 100 km/s) for others depending on the formation process; and spin up may occur not just through Roche-lobe overflow but also through wind accretion or phases of hypercritical accretion during common envelope evolution.
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