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在巨大的恒星形成星系中,快速无线电爆发的偏好

Kritti Sharma¹, Vikram Ravi^2,3, Liam Connor²

¹Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA, USA. kritti@caltech.edu.

|November 7, 2024

概括

快速无线电爆发 (FRB) 主要来自大质量,金属丰富的星系. 这表明FRB的祖先,可能是磁星,是通过这些环境中的恒星合并形成的,而不是来自单个大质量恒星.

科学领域:

天体物理学
宇宙现象

背景情况:

快速无线电爆发 (FRB) 是银河系外的一种,持续数毫秒的无线电短暂.
磁星,高度磁化的中子星,是FRB的先驱,通过观测来自银河系磁星和FRB宿主星系的恒星形成性来支持.
磁星的确切形成路径,特别是核心崩超新星 (CCSNe) 产生它们,仍然不清楚.

研究的目的:

通过分析其宿主星系的恒星群体属性来调查FRB的原始起源.
确定FRB是否是恒星形成的偏向标记,并确定影响磁星形成的潜在环境因素.

主要方法:

通过深度光学阵列 (DSA-110) 识别的30个FRB宿主星系的恒星群属性分析.
FRB宿主星系的人口统计与宇宙中的恒星形成率的比较.
对FRB宿主星系质量,金属性和潜在的祖先形成途径之间的相关性分析.

主要成果:

与宇宙恒星形成率相比,FRB宿主星系显示出大量的低质量系统.
FRB被证实是有偏见的痕迹,
在FRB宿主中恒星质量与金属度之间的正相关性表明金属度在磁星前代形成中起作用.

结论:

对大质量,金属丰富的星系的观察偏差意味着FRB祖先,可能是磁星,在有利于恒星合并的环境中形成.
金属丰富的条件可能会促进恒星的合并,导致磁星的形成,可能是通过合并残留物,而不是通过单个大质量恒星的动力发电机过程.
这些发现表明,核崩超新星的融合残余是形成FRB的磁星的关键.

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