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在二进制中子星合并残留物中,中子星陷和失衡效应
Pedro Luis Espino1,2, Peter Hammond1, David Radice1,3,4
1Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, Pennsylvania 16802, USA.
Physical review letters
|June 10, 2024
概括
中子星的合并短暂地使冷核与被困的中微子脱离了热力学平衡. 物质和中微子在几毫秒内达到平衡,限制了散射效应的活性窗口,例如散热粘度.
科学领域:
- 天体物理学 天体物理学
- 核物理 核物理 核物理
- 计算物理 计算物理
背景情况:
- 中子星的合并是极端的天体物理事件,涉及密集物质和高能中微子.
- 了解热力学平衡对于建模合并后遗留物至关重要.
- 中微子捕获及其对物质平衡的影响是研究的关键领域.
研究的目的:
- 为了研究中子星合并中的热力学平衡外效应.
- 为了确定融合残留物中物质和中微子平衡的时间表.
- 评估散热效应 (如散装粘度) 对合并结果的影响.
主要方法:
- 采用了3D一般相对论中微子辐射大模拟.
- 模拟了合并中子星的核心动态.
- 分析了残留物中的温度概况和中微子相互作用.
主要成果:
- 中子星核在合并过程中保持冷 (几MeV) 和脱离热力学平衡.
- 被捕获的中微子起源于热碰撞接口.
- 在大约2-3毫秒内,物质和中微子在剩余的大质中子星中达到平衡.
结论:
- 失衡效应是短暂的,在合并后仅持续几毫秒.
- 散射效应,如散装粘度,仅在这个短的平衡窗口中活跃.
- 模拟结果为完善中子星合并及其可观测后果模型提供了关键数据.
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