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双质中子星合并中的重元素起源于引力波事件
Daniel Kasen1,2, Brian Metzger3, Jennifer Barnes3
1Departments of Physics and Astronomy, and Theoretical Astrophysics Center, University of California, Berkeley, California 94720-7300, USA.
Nature
|November 3, 2017
概括
中子星的合并通过快速的中子捕获 (r过程) 核合成产生像黄金和这样的重元素. 这些聚变所产生的热发光,被称为千新星, 提供了宇宙元素产生的第一个直接证据.
科学领域:
- 天体物理学
- 核物理
- 宇宙学
背景情况:
- 比铁更重的元素的起源一直是天体物理学中的一个长期团.
- 理论模型表明中子星合并是快速中子捕获 (r过程) 核合成的潜在地点.
- 据预测,新合成的重元素的放射性衰变会产生千诺瓦,
研究的目的:
- 详细模拟千新星的电磁辐射.
- 为了从千诺瓦观测中推导出射出物质,速度和组成.
- 调查中子星合并在宇宙重元素生成中的作用.
主要方法:
- 开发了详细的模型来预测千诺瓦电磁辐射.
- 将模型预测与GW170817事件的光学和红外辐射数据进行比较.
- 射出物质的推断性质,包括质量,速度和元素组成.
主要成果:
- 观测到的GW170817的电磁辐射与千诺瓦相符.
- 推断出存在两个不同的喷射元件:轻型 (A < 140) 和重型 (A > 140) r过程元件.
- 喷射的质量和推断的融合率表明中子星的融合是r过程元素的主要来源.
结论:
- 中子星的合并被证实是通过r过程产生重元素的重要宇宙场所.
- 像GW170817这样的基洛诺瓦观测为重元素的核合成提供了关键的见解.
- 这项研究为分析千新星建立了一个框架, 以了解宇宙中的元素创造.
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